899 research outputs found
Extra-nuclear starbursts: Young luminous hinge clumps in interacting galaxies
Hinge clumps are luminous knots of star formation near the base of tidal features in some interacting galaxies. We use archival Hubble Space Telescope (HST) UV/optical/IR images and Chandra X-ray maps along with Galaxy Evolution Explorer UV, Spitzer IR, and ground-based optical/near-IR images to investigate the star forming properties in a sample of 12 hinge clumps in five interacting galaxies. The most extreme of these hinge clumps have star formation rates of 1-9 M ☉ yr–1, comparable to or larger than the "overlap" region of intense star formation between the two disks of the colliding galaxy system the Antennae. In the HST images, we have found remarkably large and luminous sources at the centers of these hinge clumps. These objects are much larger and more luminous than typical "super star clusters" in interacting galaxies, and are sometimes embedded in a linear ridge of fainter star clusters, consistent with star formation along a narrow caustic. These central sources have FWHM diameters of ~70 pc, compared to ~3 pc in "ordinary" super star clusters. Their absolute I magnitudes range from MI ~ – 12.2 to –16.5; thus, if they are individual star clusters they would lie near the top of the "super star cluster" luminosity function of star clusters. These sources may not be individual star clusters, but instead may be tightly packed groups of clusters that are blended together in the HST images.Comparison to population synthesis modeling indicates that the hinge clumps contain a range of stellar ages. This is consistent with expectations based on models of galaxy interactions, which suggest that star formation may be prolonged in these regions.In the Chandra images, we have found strong X-ray emission from several of these hinge clumps. In most cases, this emission is well-resolved with Chandra and has a thermal X-ray spectrum, thus it is likely due to hot gas associated with the star formation. The ratio of the extinction-corrected diffuse X-ray luminosity to the mechanical energy rate (the X-ray production efficiency) for the hinge clumps is similar to that in the Antennae galaxies, but higher than those for regions in the normal spiral galaxy NGC 2403. Two of the hinge clumps have point-like X-ray emission much brighter than expected for hot gas; these sources are likely "ultra-luminous X-ray sources" due to accretion disks around black holes. The most extreme of these sources, in Arp 240, has a hard X-ray spectrum and an absorbed X-ray luminosity of ~2 × 1041 erg s–1; this is above the luminosity expected by single high mass X-ray binaries (HMXBs), thus it may be either a collection of HMXBs or an intermediate mass black hole (≥80 M ☉)
Simple Models for Turbulent Self-Regulation in Galaxy Disks
We propose that turbulent heating, wave pressure and gas exchanges between
different regions of disks play a dominant role in determining the preferred,
quasi-equilibrium, self-similar states of gas disks on large-scales. We present
simple families of analytic, thermohydrodynamic models for these global states,
which include terms for turbulent pressure and Reynolds stresses. Star
formation rates, phase balances, and hydrodynamic forces are all tightly
coupled and balanced. The models have stratified radial flows, with the cold
gas slowly flowing inward in the midplane of the disk, and with the warm/hot
phases that surround the midplane flowing outward.
The models suggest a number of results that are in accord with observation,
as well as some novel predictions, including the following. 1) The large-scale
gas density and thermal phase distributions in galaxy disks can be explained as
the result of turbulent heating and spatial couplings. 2) The turbulent
pressures and stresses that drive radial outflows in the warm gas also allow a
reduced circular velocity there. This effect was observed by Swaters, Sancisi
and van der Hulst in NGC 891, a particularly turbulent edge-on disk. The models
predict that the effect should be universal in such disks. 3) They suggest that
a star formation rate like the phenomenological Schmidt Law is the natural
result of global thermohydrodynamical balance, and may not obtain in disks far
from equilibrium. (Abridged)Comment: 37 pages, 1 gif figure, accepted for publication in the Astrophysical
Journa
The Minimum Stellar Mass in Early Galaxies
The conditions for the fragmentation of the baryonic component during merging
of dark matter halos in the early Universe are studied. We assume that the
baryonic component undergoes a shock compression. The characteristic masses of
protostellar molecular clouds and the minimum masses of protostars formed in
these clouds decrease with increasing halo mass. This may indicate that the
initial stellar mass function in more massive galaxies was shifted towards
lower masses during the initial stages of their formation. This would result in
an increase of the number of stars per unit halo mass, i.e., the efficiency of
star formation.Comment: 18 pages, 7 figure
Models of the Morphology, Kinematics, and Star Formation History of the Prototypical Collisional Starburst System: NGC 7714/7715 = Arp 284
(abridged) We present new N-body, hydrodynamical simulations of the
interaction between the starburst galaxy NGC 7714 and its post-starburst
companion NGC 7715, focusing on the formation of the collisional features,
including: 1) the gas-rich star forming bridge, 2) the large gaseous loop (and
stellar tails) to the west of the system, 3) the very extended HI tail to the
west and north of NGC 7714, and 4) the partial stellar ring in NGC 7714. Our
simulations confirm the results of earlier work that an off-center inclined
collision between two disk galaxies is almost certainly responsible for the
peculiar morphologies of this system. However, we have explored a wider set of
initial galaxy and collisional encounter parameters than previously, and have
found a relatively narrow range of parameters that reproduce all the major
morphologies of this system. The simulations suggest specific mechanisms for
the development of several unusual structures. We find that the complex gas
bridge has up to four distinct components, with gas contributed from two sides
of NGC 7715, as well as from NGC 7714. The observed gas-star offset in this
bridge is accounted for in the simulations by the dissipative evolution of the
gas. The models also indicate that the low surface brightness HI tail to the
far west of NGC 7714 is the end of the NGC 7715 countertail, curved behind the
two galaxies. Spectral evolutionary models of the NGC 7714 core by Lan\c{c}on
et al. suggest the possibility of multiple starbursts in the last 300 Myr. Our
hydrodynamic models suggest that bursts could be triggered by induced ring-like
waves, and a post-collision buildup of gas in the core of the galaxy.Comment: 24 pages, 20 figures, accepted for ApJ Supp
Atomic Hydrogen and Star Formation in the Bridge/Ring Interacting Galaxy Pair NGC 7714/7715 (Arp 284)
We present high spatial resolution 21 cm HI maps of the interacting galaxy
pair NGC 7714/7715. We detect a massive (2 x 10**9 M(sun)) HI bridge connecting
the galaxies that is parallel to but offset from the stellar bridge. A chain of
HII regions traces the gaseous bridge, with H-alpha peaks near but not on the
HI maxima. An HI tidal tail is also detected to the east of the smaller galaxy
NGC 7715, similarly offset from a stellar tail. The strong partial stellar ring
on the eastern side of NGC 7714 has no HI counterpart, but on the opposite side
of NGC 7714 there is a 10**9 M(sun) HI loop 11 kpc in radius. Within the NGC
7714 disk, clumpy HI gas is observed associated with star formation regions.
Redshifted HI absorption is detected towards the starburst nucleus. We compare
the observed morphology and gas kinematics with gas dynamical models in which a
low-mass companion has an off-center prograde collision with the outer disk of
a larger galaxy. These simulations suggest that the bridge in NGC 7714/7715 is
a hybrid between bridges seen in systems like M51 and the purely gaseous
`splash' bridges found in ring galaxies like the Cartwheel. The offset between
the stars and gas in the bridge may be due to dissipative cloud-cloud
collisions occuring during the impact of the two gaseous disks.Comment: 31 pages, Latex, 11 figures, to be published in the July 10, 1997
issue of the Astrophysical Journa
Galaxy Collisions - Dawn of a New Era
The study of colliding galaxies has progressed rapidly in the last few years,
driven by observations with powerful new ground and space-based instruments.
These instruments have used for detailed studies of specific nearby systems,
statistical studies of large samples of relatively nearby systems, and
increasingly large samples of high redshift systems. Following a brief summary
of the historical context, this review attempts to integrate these studies to
address the following key issues. What role do collisions play in galaxy
evolution, and how can recently discovered processes like downsizing resolve
some apparently contradictory results of high redshift studies? What is the
role of environment in galaxy collisions? How is star formation and nuclear
activity orchestrated by the large scale dynamics, before and during merger?
Are novel modes of star formation involved? What are we to make of the
association of ultraluminous X-ray sources with colliding galaxies? To what do
degree do mergers and feedback trigger long-term secular effects? How far can
we push the archaeology of individual systems to determine the nature of
precursor systems and the precise effect of the interaction? Tentative answers
to many of these questions have been suggested, and the prospects for answering
most of them in the next few decades are good.Comment: 44 pages, 9 figures, review article in press for Astrophysics Update
Vol.
Sex differences in the association between plasma copeptin and incident type 2 diabetes: the Prevention of Renal and Vascular Endstage Disease (PREVEND) study
AIMS/HYPOTHESIS: Vasopressin plays a role in osmoregulation, glucose homeostasis and inflammation. Therefore, plasma copeptin, the stable C-terminal portion of the precursor of vasopressin, has strong potential as a biomarker for the cardiometabolic syndrome and diabetes. Previous results were contradictory, which may be explained by differences between men and women in responsiveness of the vasopressin system. The aim of this study was to evaluate the usefulness of copeptin for prediction of future type 2 diabetes in men and women separately. METHODS: From the Prevention of Renal and Vascular Endstage Disease (PREVEND) study, 4,063 women and 3,909 men without diabetes at baseline were included. A total of 208 women and 288 men developed diabetes during a median follow-up of 7.7 years. RESULTS: In multivariable-adjusted models, we observed a stronger association of copeptin with risk of future diabetes in women (OR 1.49 [95% CI 1.24, 1.79]) than in men (OR 1.01 [95% CI 0.85, 1.19]) (p (interaction) < 0.01). The addition of copeptin to the Data from the Epidemiological Study on the Insulin Resistance Syndrome (DESIR) clinical model improved the discriminative value (C-statistic,+0.007, p = 0.02) and reclassification (integrated discrimination improvement [IDI] = 0.004, p < 0.01) in women. However, we observed no improvement in men. The additive value of copeptin in women was maintained when other independent predictors, such as glucose, high sensitivity C-reactive protein (hs-CRP) and 24 h urinary albumin excretion (UAE), were included in the model. CONCLUSIONS/INTERPRETATION: The association of plasma copeptin with the risk of developing diabetes was stronger in women than in men. Plasma copeptin alone, and along with existing biomarkers (glucose, hs-CRP and UAE), significantly improved the risk prediction for diabetes in women
The Molecule-Rich Tail of the Peculiar Galaxy NGC 2782 (Arp 215)
We present the first detection of a large quantity of molecular gas in the
extended tail of an interacting galaxy. Using the NRAO 12m telescope, we have
detected CO (1 - 0) at five locations in the eastern tail of the peculiar
starburst galaxy NGC 2782. The CO velocities and narrow (FWHM = 50 km/s) line
widths in these positions agree with those seen in HI, confirming that the
molecular gas is indeed associated with the tail rather than the main disk. As
noted previously, the gas in this tail has an apparent `counter-rotation'
compared to gas in the core of the galaxy, probably because the tails do not
lie in the same plane as the disk. Assuming the standard Galactic conversion
N(H2)/I(CO) factor, these observations indicate a total molecular gas mass of 6
X 10**8 M(sun) in this tail. This may be an underestimate of the total H2 mass
if the gas is metal-poor. This molecular gas mass, and the implied H2/HI mass
ratio of 0.6, are higher than that found in many dwarf irregular galaxies.
Comparison with an available H-alpha map of this galaxy, however, shows that
the rate of star formation in this feature is extremely low relative to the
available molecular gas, compared to L(H-alpha)/M(H2) values for both spiral
and irregular galaxies. Thus the timescale for depletion of the gas in this
feature is very long.Comment: 19 pages, 6 figures, Latex. To appear in the Astronomical Journa
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