2,171 research outputs found
Quasi-isometric groups with no common model geometry
A simple surface amalgam is the union of a finite collection of surfaces with
precisely one boundary component each and which have their boundary curves
identified. We prove if two fundamental groups of simple surface amalgams act
properly and cocompactly by isometries on the same proper geodesic metric
space, then the groups are commensurable. Consequently, there are infinitely
many fundamental groups of simple surface amalgams that are quasi-isometric,
but which do not act properly and cocompactly on the same proper geodesic
metric space.Comment: v2: 19 pages, 6 figures; minor changes. To appear in Journal of the
London Mathematical Societ
Hyperbolic groups that are not commensurably coHopfian
Sela proved every torsion-free one-ended hyperbolic group is coHopfian. We
prove that there exist torsion-free one-ended hyperbolic groups that are not
commensurably coHopfian. In particular, we show that the fundamental group of
every simple surface amalgam is not commensurably coHopfian.Comment: v3: 14 pages, 4 figures; minor changes. To appear in International
Mathematics Research Notice
How to recognize opportunities: Heterarchical search in a Wall Street trading room
Our task in this paper is to analyze the organization of trading in the era of quantitative finance. To do so, we conduct an ethnography of arbitrage, the trading strategy that best exemplifies finance in the wake of the quantitative revolution. In contrast to value and momentum investing, we argue, arbitrage involves an art of association - the construction of equivalence (comparability) of properties across different assets. In place of essential or relationa l characteristics, the peculiar valuation that takes place in arbitrage is based on an operation that makes something the measure of something else - associating securities to each other. The process of recognizing opportunities and the practices of making novel associations are shaped by the specific socio-spatial and socio-technical configurations of the trading room. Calculation is distributed across persons and instruments as the trading room organizes interaction among diverse principles of valuation.Arbitrage, trading, heterarchy
Resolving identities: Successive crises in a trading room after 9/11
How do organizations cope with extreme uncertainty? The existing literature is divided on this issue: some argue that organizations deal best with uncertainty in the environment by reproducing it in the organization, whereas others contend that the orga nization should be protected from the environment. In this paper we study the case of a Wall Street investment bank that lost its entire office and trading technology in the terrorist attack of September 11 th. The traders survived, but were forced to relocate to a makeshift trading room in New Jersey. During the six months the traders spent outside New York City, they had to deal with fears and insecurities inside the company as well as outside it: anxiety about additional attacks, questions of professional identity, doubts about the future of the firm, and ambiguities about the future re-location of the trading room. The firm overcame these uncertainties by protecting the traders’ identities and their ability to engage in sensemaking. The organization held together through a leadership style that managed ambiguities and created the conditions for new solutions to emerge.Organizational responsiveness, uncertainty, september 11th
Effects of self-consistent rest-ultraviolet colours in semi-empirical galaxy formation models
Connecting the observed rest-ultraviolet (UV) luminosities of high-
galaxies to their intrinsic luminosities (and thus star formation rates)
requires correcting for the presence of dust. We bypass a common
dust-correction approach that uses empirical relationships between infrared
(IR) emission and UV colours, and instead augment a semi-empirical model for
galaxy formation with a simple -- but self-consistent -- dust model and use it
to jointly fit high- rest-UV luminosity functions (LFs) and colour-magnitude
relations (-). In doing so, we find that UV colours
evolve with redshift (at fixed UV magnitude), as suggested by observations,
even in cases without underlying evolution in dust production, destruction,
absorption, or geometry. The observed evolution in our model arises due to the
reduction in the mean stellar age and rise in specific star formation rates
with increasing . The UV extinction, , evolves similarly
with redshift, though we find a systematically shallower relation between
and than that predicted by IRX-
relationships derived from galaxy samples. Finally, assuming that
high transmission () is a reliable LAE indicator,
modest scatter in the effective dust surface density of galaxies can explain
the evolution both in - and LAE fractions. These
predictions are readily testable by deep surveys with the James Webb Space
Telescope.Comment: 14+4 pages, 11+5 figures, accepted for publication in MNRA
Keck Spectroscopy of Faint 3 < z < 7 Lyman Break Galaxies: III. The Mean Ultraviolet Spectrum at z=4
We present and discuss the mean rest-frame ultraviolet spectrum for a sample
of 81 Lyman Break Galaxies (LBGs) selected to be B-band dropouts with a mean
redshift of z=3.9 and apparent magnitudes z_AB<26. Most of the individual
spectra are drawn from our ongoing survey in the GOODS fields with the Keck
DEIMOS spectrograph, and we have augmented our sample with published data taken
with FORS2 on the VLT. In general we find similar trends in the spectral
diagnostics to those found in the earlier, more extensive survey of LBGs at z=3
undertaken by Shapley et al (2003). Specifically, we find low-ionization
absorption lines which trace the presence of neutral outflowing gas are weaker
in galaxies with stronger Lyman-alpha emission, bluer UV spectral slopes, lower
stellar masses, lower UV luminosities and smaller half-light radii. This is
consistent with a physical picture whereby star formation drives outflows of
neutral gas which scatters Lyman-alpha and gives rise to strong low-ionization
absorption lines, while increasing the stellar mass, size, metallicity, and
dust content of galaxies. Typical galaxies are thus expected to have stronger
Lyman-alpha emission and weaker low-ionization absorption at earlier times
(higher redshifts). Indeed, our mean spectrum at z=4 shows somewhat weaker
low-ionization absorption lines than at z=3 and available data at higher
redshift indicates a rapid decrease in low-ionization absorption strength with
redshift. We argue that the reduced low-ionization absorption is likely caused
by a decrease in the covering fraction and/or velocity range of outflowing
neutral gas at earlier epochs. Our continuing survey will enable us to extend
these diagnostics more reliably to higher redshift and determine the
implications for the escape fraction of ionizing photons which governs the role
of early galaxies in cosmic reionization. [Abridged]Comment: 17 pages, 12 figures, submitted to ApJ. Comments welcom
Keck Spectroscopy of Faint 3<z<7 Lyman Break Galaxies:- II. A High Fraction of Line Emitters at Redshift Six
As Lyman-alpha photons are scattered by neutral hydrogen, a change with
redshift in the Lyman-alpha equivalent width distribution of distant galaxies
offers a promising probe of the degree of ionization in the intergalactic
medium and hence when cosmic reionization ended. This simple test is
complicated by the fact that Lyman-alpha emission can also be affected by the
evolving astrophysical details of the host galaxies. In the first paper in this
series, we demonstrated both a luminosity and redshift dependent trend in the
fraction of Lyman-alpha emitters seen within color-selected Lyman-break
galaxies (LBGs) over the range 3<z<6; lower luminosity galaxies and those at
higher redshift show an increased likelihood of strong emission. Here we
present the results from much deeper 12.5 hour exposures with the Keck DEIMOS
spectrograph focused primarily on LBGs at z~6 which enable us to confirm the
redshift dependence of line emission more robustly and to higher redshift than
was hitherto possible. We find 54+/-11% of faint z~6 LBGs show strong (W_0>25
A) emission, an increase of 1.6x from a similar sample observed at z~4. With a
total sample of 74 z~6 LBGs, we determine the luminosity-dependent Lyman-alpha
equivalent width distribution. Assuming continuity in these trends to the new
population of z~7 sources located with the Hubble WFC3/IR camera, we predict
that unless the neutral fraction rises in the intervening 200 Myr, the success
rate for spectroscopic confirmation using Lyman-alpha emission should be high.Comment: 6 pages, 3 figures, submitted to ApJ
The [OIII]H Equivalent Width Distribution at z7: Implications for the Contribution of Galaxies to Reionization
We quantify the distribution of [OIII]+H line strengths at z7
using a sample of 20 bright (M 21) galaxies. We
select these systems over wide-area fields (2.3 deg total) using a new
colour-selection which precisely selects galaxies at z6.636.83, a
redshift range where blue Spitzer/IRAC [3.6][4.5] colours unambiguously
indicate strong [OIII]H emission. These 20 galaxies suggest a
log-normal [OIII]H EW distribution with median EW =
759 and standard deviation =
0.26 dex. We find no evidence for strong variation in this EW
distribution with UV luminosity. The typical [OIII]+H EW at z7
implied by our sample is considerably larger than that in massive star forming
galaxies at z2, consistent with a shift toward larger average sSFR (4.4
Gyr) and lower metallicities (0.16 Z). We also find evidence for
the emergence of a population with yet more extreme nebular emission
([OIII]+H EW1200 ) that is rarely seen at
lower redshifts. These objects have extremely large sSFR (30 Gyr), as
would be expected for systems undergoing a burst or upturn in star formation.
While this may be a short-lived phase, our results suggest that 20% of the
z7 population has such extreme nebular emission, implying that galaxies
likely undergo intense star formation episodes regularly at z6. We argue
that this population may be among the most effective ionizing agents in the
reionization era, both in terms of photon production efficiency and escape
fraction. We furthermore suggest that galaxies passing through this large sSFR
phase are likely to be very efficient in forming bound star clusters.Comment: 20 pages, 11 figures. Accepted in MNRAS with minor revision
High-redshift galaxies and black holes in the eyes of JWST: a population synthesis model from infrared to X-rays
The first billion years of the Universe is a pivotal time: stars, black holes
(BHs) and galaxies form and assemble, sowing the seeds of galaxies as we know
them today. Detecting, identifying and understand- ing the first galaxies and
BHs is one of the current observational and theoretical challenges in galaxy
formation. In this paper we present a population synthesis model aimed at
galaxies, BHs and Active Galactic Nuclei (AGNs) at high redshift. The model
builds a population based on empirical relations. Galaxies are characterized by
a spectral energy distribution determined by age and metallicity, and AGNs by a
spectral energy distribution determined by BH mass and accretion rate. We
validate the model against observational constraints, and then predict
properties of galaxies and AGN in other wavelength and/or luminosity ranges,
estimating the contamination of stellar populations (normal stars and high-mass
X-ray binaries) for AGN searches from the infrared to X-rays, and vice-versa
for galaxy searches. For high-redshift galaxies, with stellar ages < 1 Gyr, we
find that disentangling stellar and AGN emission is challenging at restframe
UV/optical wavelengths, while high-mass X-ray binaries become more important
sources of confusion in X-rays. We propose a color-color selection in JWST
bands to separate AGN vs star-dominated galaxies in photometric observations.
We also esti- mate the AGN contribution, with respect to massive, hot,
metal-poor stars, at driving high ionization lines, such as C IV and He II.
Finally, we test the influence of the minimum BH mass and occupa- tion fraction
of BHs in low mass galaxies on the restframe UV/near-IR and X-ray AGN
luminosity function.Comment: Accepted for publication in the Astrophysical Journa
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