453 research outputs found
The Cognitive Psychology of Humour in Written Puns
The primary purpose of this dissertation was to investigate how humour from written puns is produced. Prior models have emphasized that novel or surprising incongruities should be important to humour appreciation (Suls, 1972; Topolinski, 2014). In study 1, a new approach to operationalizing incongruity as semantic dissimilarity was developed and tested using Latent Semantic Analysis (Landauer, Foltz & Laham, 1998). “Latent semantic incongruity” was associated with humour ratings, but only for puns with low ratings of familiarity from a prior occasion or for those with a low level of aggressive content. Overall, there was also an unexpected strong positive association between familiarity with a pun from a prior occasion and humour ratings. Study 2 demonstrated that humour ratings for puns decreases with repeated exposures. Changes in humour with repetition were dependent on latent semantic incongruity, the duration of time spent comprehending the pun and providing humour ratings, and on how humour was measured. Study 3 investigated whether “elaboration” on the two implied concepts in each pun was associated with humour (as predicted by Wyer & Collins, 1992). Elaboration quantity (the number of associated words that participants could comfortably list) and elaboration duration (the duration of time participants spent on the elaboration task) were associated with humour ratings, but only for familiar puns. In summary, fluent comprehension of incongruity was important to humour from unfamiliar puns, whereas elaboration on the implied concepts in puns was important to humour appreciation for puns that were familiar from a prior occasion
PRAGMATICS OF IRONIC CRITICISM
Previous studies have demonstrated that ironic criticism can either dilute or enhance a message and that it may provide a mnemonic advantage. This thesis investigated whether irony dilutes or enhances ironic criticism as a function of contrast or speaker orientation (whether an interpreter concentrates on speaker intention or social impact). Participants were asked to interpret the functions of direct and ironic criticisms in short written scenarios which each described a friendly conversation (study 1) or an argument (study 2) between close, same gender friends. Ratings of ironic criticism were not dependent on either contrast or interpreter orientation, nor was there evidence of a mnemonic advantage for ironic expression. Irony caused criticism to appear more mocking (enhancing the criticism of the message), while simultaneously causing the message to appear more humorous, polite, and less negative than direct expression (diluting negative regard in the message). Theoretical implications are discusse
The Effect of Shifts in Reward Magnitude and Changes of Schedule of Reinforcement on Resistance to Extinction
The problem concerned the resistance to extinction of an alley running response as a function of various combinations of reward sizes (l or 10 pellets) and schedules of reinforcement (50 or 100%). Three experimental phases were used (acquisition, shift of reward, and extinction). Three measures were taken in the alley (start, alley, and goal speed). Animals trained under partial reinforcement (PRF) showed no significant differences in acquisition running speed over animals trained on continuous reinforcement (CRF). Depression effects (decreases in running speed) were observed for both CRF and PRF trained animals during the shift phase. Overall tests between PRF and CRF groups revealed no significant differences in number of trials to extinction. The results were discussed in terms of operant conditioning theory. Ideas for further research involving shift periods of varying lengths were offered
Near-Field Limits on the Role of Faint Galaxies in Cosmic Reionization
Reionizing the Universe with galaxies appears to require significant star
formation in low-mass halos at early times, while local dwarf galaxy counts
tell us that star formation has been minimal in small halos around us today.
Using simple models and the ELVIS simulation suite, we show that reionization
scenarios requiring appreciable star formation in halos with at are in serious tension with galaxy counts
in the Local Group. This tension originates from the seemingly inescapable
conclusion that 30 - 60 halos with at
will survive to be distinct bound satellites of the Milky Way at .
Reionization models requiring star formation in such halos will produce dozens
of bound galaxies in the Milky Way's virial volume today (and 100 - 200
throughout the Local Group), each with of old stars
( Gyr). This exceeds the stellar mass function of classical Milky
Way satellites today, even without allowing for the (significant)
post-reionization star formation observed in these galaxies. One possible
implication of these findings is that star formation became sharply inefficient
in halos smaller than at early times, implying that the
high- luminosity function must break at magnitudes brighter than is often
assumed (at ). Our results suggest that JWST (and
possibly even HST with the Frontier Fields) may realistically detect the
faintest galaxies that drive reionization. It remains to be seen how these
results can be reconciled with the most sophisticated simulations of early
galaxy formation at present, which predict substantial star formation in
halos during the epoch of reionization.Comment: 6 pages, 4 figures; minor updates. Published in MNRAS Letter
ELVIS: Exploring the Local Volume in Simulations
We introduce a set of high-resolution dissipationless simulations that model
the Local Group (LG) in a cosmological context: Exploring the Local Volume in
Simulations (ELVIS). The suite contains 48 Galaxy-size halos, each within
high-resolution volumes that span 2-5 Mpc in size, and each resolving thousands
of systems with masses below the atomic cooling limit. Half of the ELVIS galaxy
halos are in paired configurations similar to the Milky Way (MW) and M31; the
other half are isolated, mass-matched analogs. We find no difference in the
abundance or kinematics of substructure within the virial radii of isolated
versus paired hosts. On Mpc scales, however, LG-like pairs average almost twice
as many companions and the velocity field is kinematically hotter and more
complex. We present a refined abundance matching relation between stellar mass
and halo mass that reproduces the observed satellite stellar mass functions of
the MW and M31 down to the regime where incompleteness is an issue, . Within a larger region spanning approximately 3
Mpc, the same relation predicts that there should be 1000 galaxies with
awaiting discovery. We show that up to 50% of halos
within 1 Mpc of the MW or M31 could be systems that have previously been within
the virial radius of either giant. By associating never-accreted halos with
gas-rich dwarfs, we show that there are plausibly 50 undiscovered dwarf
galaxies with HI masses within the Local Volume. The radial
velocity distribution of these predicted gas-rich dwarfs can be used to inform
follow-up searches based on ultra-compact high-velocity clouds found in the
ALFALFA survey.Comment: 22 pages, 19 figures, 3 tables; v2 -- accepted to MNRAS. Movies,
images, and data are available at http://localgroup.ps.uci.edu/elvi
On the stark difference in satellite distributions around the Milky Way and Andromeda
We compare spherically-averaged radial number counts of bright (> 10^5 Lsun)
dwarf satellite galaxies within 400 kpc of the Milky Way (MW) and M31 and find
that the MW satellites are much more centrally concentrated. Remarkably, the
two satellite systems are almost identical within the central 100 kpc, while
M31 satellites outnumber MW satellites by about a factor of four at deprojected
distances spanning 100 - 400 kpc. We compare the observed distributions to
those predicted for LCDM suhbalos using a suite of 44 high-resolution ~10^12
halo zoom simulations, 22 of which are in pairs like the MW and M31. We find
that the radial distribution of satellites around M31 is fairly typical of
those predicted for subhalos, while the Milky Way's distribution is more
centrally concentrated that any of our simulated LCDM halos. One possible
explanation is that our census is bright (> 10^5 Lsun) MW dwarf galaxies is
significantly incomplete beyond ~ 100 kpc of the Sun. If there were ~8 - 20
more bright dwarfs orbiting undetected at 100 - 400 kpc, then the Milky Way's
radial distribution would fall within the range expected from subhalo
distributions and alos look very much like the known M31 system. We use our
simulations to demonstrate that there is enough area left unexplored by the
Sloan Digital Sky Survey and its extensions that the discovery of ~10 new
bright dwarfs is not implausible given the expected range of angular anisotropy
of subhalos in the sky.Comment: 10 pages, 8 figures, submitted to MNRA
Organized Chaos: Scatter in the relation between stellar mass and halo mass in small galaxies
We use Local Group galaxy counts together with the ELVIS N-body simulations
to explore the relationship between the scatter and slope in the stellar mass
vs. halo mass relation at low masses, .
Assuming models with log-normal scatter about a median relation of the form
, the preferred log-slope steepens from
in the limit of zero scatter to in the
case of dex of scatter in at fixed halo mass. We provide fitting
functions for the best-fit relations as a function of scatter, including cases
where the relation becomes increasingly stochastic with decreasing mass. We
show that if the scatter at fixed halo mass is large enough ( dex)
and if the median relation is steep enough (), then the
"too-big-to-fail" problem seen in the Local Group can be self-consistently
eliminated in about of realizations. This scenario requires that
the most massive subhalos host unobservable ultra-faint dwarfs fairly often; we
discuss potentially observable signatures of these systems. Finally, we compare
our derived constraints to recent high-resolution simulations of dwarf galaxy
formation in the literature. Though simulation-to-simulation scatter in
at fixed is large among separate authors (
dex), individual codes produce relations with much less scatter and usually
give relations that would over-produce local galaxy counts.Comment: 15 pages, 6 figures, 1 table. Accepted for publication into MNRA
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