267 research outputs found
Simulated Annealing for JPEG Quantization
JPEG is one of the most widely used image formats, but in some ways remains
surprisingly unoptimized, perhaps because some natural optimizations would go
outside the standard that defines JPEG. We show how to improve JPEG compression
in a standard-compliant, backward-compatible manner, by finding improved
default quantization tables. We describe a simulated annealing technique that
has allowed us to find several quantization tables that perform better than the
industry standard, in terms of both compressed size and image fidelity.
Specifically, we derive tables that reduce the FSIM error by over 10% while
improving compression by over 20% at quality level 95 in our tests; we also
provide similar results for other quality levels. While we acknowledge our
approach can in some images lead to visible artifacts under large
magnification, we believe use of these quantization tables, or additional
tables that could be found using our methodology, would significantly reduce
JPEG file sizes with improved overall image quality.Comment: Appendix not included in arXiv version due to size restrictions. For
full paper go to:
http://www.eecs.harvard.edu/~michaelm/SimAnneal/PAPER/simulated-annealing-jpeg.pd
The mass-metallicity gradient relation of early-type galaxies
We present a newly observed relation between galaxy mass and radial
metallicity gradients of early-type galaxies. Our sample of 51 early-type
galaxies encompasses a comprehensive mass range from dwarf to brightest cluster
galaxies. The metallicity gradients are measured out to one effective radius by
comparing nearly all of the Lick absorption-line indices to recent models of
single stellar populations. The relation shows very different behaviour at low
and high masses, with a sharp transition being seen at a mass of ~ 3.5 x 10^10
M_sun (velocity dispersion of ~140 km/s, M_B ~ -19). Low-mass galaxies form a
tight relation with mass, such that metallicity gradients become shallower with
decreasing mass and positive at the very low-mass end. Above the mass
transition point several massive galaxies have steeper gradients, but a clear
downturn is visible marked by a broad scatter. The results are interpreted in
comparison with competing model predictions. We find that an early star-forming
collapse could have acted as the main mechanism for the formation of low-mass
galaxies, with star formation efficiency increasing with galactic mass. The
high-mass downturn could be a consequence of merging and the observed larger
scatter a natural result of different merger properties. These results suggest
that galaxies above the mass threshold of ~ 3.5 x 10^10 M_sun might have formed
initially by mergers of gas-rich disc galaxies and then subsequently evolved
via dry merger events. The varying efficiency of the dissipative merger-induced
starburst and feedback processes have shaped the radial metallicity gradients
in these high-mass systems.Comment: 5 pageg, 3 figures, accepted by ApJ Lette
Adaptive Optics Imaging of QSOs with Double-Peaked Narrow Lines: Are they Dual AGNs?
Active galaxies hosting two accreting and merging super-massive black holes
(SMBHs) -- dual Active Galactic Nuclei (AGN) -- are predicted by many current
and popular models of black hole-galaxy co-evolution. We present here the
results of a program that has identified a set of probable dual AGN candidates
based on near Infra-red (NIR) Laser Guide-Star Adaptive Optics (LGS AO) imaging
with the Keck II telescope. These candidates are selected from a complete
sample of radio-quiet Quasi-stellar Objects (QSOs) drawn from the Sloan Digital
Sky Survey (SDSS), which show double-peaked narrow AGN emission lines. Of the
twelve AGNs imaged, we find six with double galaxy structure, of which four are
in galaxy mergers. We measure the ionization of the two velocity components in
the narrow AGN lines to test the hypothesis that both velocity components come
from an active nucleus. The combination of a well-defined parent sample and
high-quality imaging allows us to place constraints on the fraction of SDSS
QSOs that host dual accreting black holes separated on kiloparsec (kpc) scales:
~0.3%-0.65%. We derive from this fraction the time spent in a QSO phase during
a typical merger and find a value that is much lower than estimates that arise
from QSO space densities and galaxy merger statistics. We discuss possible
reasons for this difference. Finally, we compare the SMBH mass distributions of
single and dual AGN and find little difference between the two within the
limited statistics of our program, hinting that most SMBH growth happens in the
later stages of a merger process.Comment: 9 pages, 4 figures, 1 table; accepted to the Astrophysical Journa
Eigenstripping, Spectral Decay, and Edge-Expansion on Posets
Fast mixing of random walks on hypergraphs (simplicial complexes) has recently led to myriad breakthroughs throughout theoretical computer science. Many important applications, however, (e.g. to LTCs, 2-2 games) rely on a more general class of underlying structures called posets, and crucially take advantage of non-simplicial structure. These works make it clear that the global expansion properties of posets depend strongly on their underlying architecture (e.g. simplicial, cubical, linear algebraic), but the overall phenomenon remains poorly understood. In this work, we quantify the advantage of different poset architectures in both a spectral and combinatorial sense, highlighting how regularity controls the spectral decay and edge-expansion of corresponding random walks.
We show that the spectra of walks on expanding posets (Dikstein, Dinur, Filmus, Harsha APPROX-RANDOM 2018) concentrate in strips around a small number of approximate eigenvalues controlled by the regularity of the underlying poset. This gives a simple condition to identify poset architectures (e.g. the Grassmann) that exhibit strong (even exponential) decay of eigenvalues, versus architectures like hypergraphs whose eigenvalues decay linearly - a crucial distinction in applications to hardness of approximation and agreement testing such as the recent proof of the 2-2 Games Conjecture (Khot, Minzer, Safra FOCS 2018). We show these results lead to a tight characterization of edge-expansion on expanding posets in the ??-regime (generalizing recent work of Bafna, Hopkins, Kaufman, and Lovett (SODA 2022)), and pay special attention to the case of the Grassmann where we show our results are tight for a natural set of sparsifications of the Grassmann graphs. We note for clarity that our results do not recover the characterization of expansion used in the proof of the 2-2 Games Conjecture which relies on ?_? rather than ??-structure
Mass of the Southern Black Hole in NGC 6240 from Laser Guide Star Adaptive Optics
NGC 6240 is a pair of colliding disk galaxies, each with a black hole in its
core. We have used laser guide star adaptive optics on the Keck II telescope to
obtain high-resolution (") near-infrared integral-field spectra of
the region surrounding the supermassive black hole in the south nucleus of this
galaxy merger. We use the K-band CO absorption bandheads to trace stellar
kinematics. We obtain a spatial resolution of about 20 pc and thus directly
resolve the sphere of gravitational influence of the massive black hole. We
explore two different methods to measure the black hole mass. Using a Jeans
Axisymmetric Multi-Gaussian mass model, we investigate the limit that a relaxed
mass distribution produces all of the measured velocity dispersion, and find an
upper limit on the black hole mass at 2.0 \pm 0.2 \times 10^9 M_{\sun}. When
assuming the young stars whose spectra we observe remain in a thin disk, we
compare Keplerian velocity fields to the measured two-dimensional velocity
field measured and fit for a mass profile containing a black hole point mass
plus a radially-varying spherical component, which suggests a lower limit for
the black hole mass of 8.7 \pm 0.3 \times 10^8 M_{\sun}. Our measurements of
the stellar velocity dispersion place this AGN within the scatter of the
- relation. As NGC 6240 is a merging system, this may
indicate that the relation is preserved during a merger at least until the
final coalescence of the two nuclei.Comment: 10 pages, 12 figures; accepted to Ap
Particle Concentration Characterization for Jet Engine Emissions under Cruise Conditions
Airborne particle measurements during NASA project SUCCESS have shown that particle concentration profiles serve as good indicators of aircraft exhaust plume encounters. During exhaust plume penetrations there is a strong anticorrelation between the ratio of nonvolatile/total particulates and Nitrogen Oxide (NO) concentrations. an increase in fuel sulfur content was found to increase the total particle emission index, while the nonvolatile emission index remained unchanged. the EI\u27s increased by a factor of 2.6 as the fuel sulfur increased from 70 - 700 ppm. the large particle size distribution (200-400 nm) was seen as a good long term indicator of an aircraft exhaust plume. Airborne particle measurements during NASA project SUCCESS have shown that particle concentration profiles serve as good indicators of aircraft exhaust plume encounters. During exhaust plume penetrations there is a strong anticorrelation between the ratio of nonvolatile/total particulates and Nitrogen Oxide (NO) concentrations. an increase in fuel sulfur content was found to increase the total particle emission index, while the nonvolatile emission index remained unchanged. the EI\u27s increased by a factor of 2.6 as the fuel sulfur increased from 70-700 ppm. the large particle size distribution (200-400 nm) was seen as a good long term indicator of an aircraft exhaust plume
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