자연주의적 탐구조사(Naturalistic Inquiry)

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Using Multivariate Statistics

Preface to the Princeton Landmarks in Biology Edition vii Preface xi Symbols Used xiii 1. The Importance of Islands 3 2. Area and Number of Speicies 8 3. Further Explanations of the Area-Diversity Pattern 19 4. The Strategy of Colonization 68 5. Invasibility and the Variable Niche 94 6. Stepping Stones and Biotic Exchange 123 7. Evolutionary Changes Following Colonization 145 8. Prospect 181 Glossary 185 References 193 Index 201

The Theory of Island Biogeography

We review recent determinations of the present-day mass function (PDMF) and initial mass function (IMF) in various components of the Galaxy—disk, spheroid, young, and globular clusters—and in conditions characteristic of early star formation. As a general feature, the IMF is found to depend weakly on the environment and to be well described by a power-law form forM , and a lognormal form below, except possibly for m!1 early star formation conditions. The disk IMF for single objects has a characteristic mass around M , m!0.08 c and a variance in logarithmic mass , whereas the IMF for multiple systems hasM , and . j!0.7 m!0.2 j!0.6 c The extension of the single MF into the brown dwarf regime is in good agreement with present estimates of L- and T-dwarf densities and yields a disk brown dwarf number density comparable to the stellar one, n!n! BD " pc !3 .T he IMF of young clusters is found to be consistent with the disk fi eld IMF, providing the same correction 0.1 for unresolved binaries, confirming the fact that young star clusters and disk field stars represent the same stellar population. Dynamical effects, yielding depletion of the lowest mass objects, are found to become consequential for ages!130 Myr. The spheroid IMF relies on much less robust grounds. The large metallicity spread in the local subdwarf photometric sample, in particular, remains puzzling. Recent observations suggest that there is a continuous kinematic shear between the thick-disk population, present in local samples, and the genuine spheroid one. This enables us to derive only an upper limit for the spheroid mass density and IMF. Within all the uncertainties, the latter is found to be similar to the one derived for globular clusters and is well represented also by a lognormal form with a characteristic mass slightly larger than for the disk, M , ,e xcluding as ignif icant population of m!0.2-0.3 c brown dwarfs in globular clusters and in the spheroid. The IMF characteristic of early star formation at large redshift remains undetermined, but different observational constraints suggest that it does not extend below!1M , .T hese results suggest a characteristic mass for star formation that decreases with time, from conditions prevailing at large redshift to conditions characteristic of the spheroid (or thick disk) to present-day conditions.Theseconclusions,however, remain speculative, given the large uncertainties in the spheroid and early star IMF determinations. These IMFs allow a reasonably robust determination of the Galactic present-day and initial stellar and brown dwarf contents. They also have important galactic implications beyond the Milky Way in yielding more accurate mass-to-light ratio determinations. The mass-to-light ratios obtained with the disk and the spheroid IMF yield values 1.8-1.4 times smaller than for a Salpeter IMF, respectively, in agreement with various recent dynamical determinations. This general IMF determination is examined in the context of star formation theory. None of the theories based on a Jeans-type mechanism, where fragmentation is due only to gravity, can fulfill all the observational constraints on star formation and predict a large number of substellar objects. On the other hand, recent numerical simulations of compressible turbulence, in particular in super-Alfvenic conditions, seem to reproduce both qualitatively and quantitatively the stellar and substellar IMF and thus provide an appealing theoretical foundation. In this picture, star formation is induced by the dissipation of large-scale turbulence to smaller scales through radiative MHD shocks, producing filamentary structures. These shocks produce local nonequilibrium structures with large density contrasts, which collapse eventually in gravitationally bound objects under the combined influence of turbulence and gravity. The concept of a single Jeans mass is replaced by a distribution of local Jeans masses, representative of the lognormal probability density function of the turbulent gas. Objects below the mean thermal Jeans mass still have a possibility to collapse, although with a decreasing probability.

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Galactic stellar and substellar initial mass function

In the 1980s, exosomes were described as vesicles of endosomal origin secreted from reticulocytes. Interest increased around these extracellular vesicles, as they appeared to participate in several cellular processes. Exosomes bear proteins, lipids, and RNAs, mediating intercellular communication between different cell types in the body, and thus affecting normal and pathological conditions. Only recently, scientists acknowledged the difficulty of separating exosomes from other types of extracellular vesicles, which precludes a clear attribution of a particular function to the different types of secreted vesicles. To shed light into this complex but expanding field of science, this review focuses on the definition of exosomes and other secreted extracellular vesicles. Their biogenesis, their secretion, and their subsequent fate are discussed, as their functions rely on these important processes.

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Biogenesis, Secretion, and Intercellular Interactions of Exosomes and Other Extracellular Vesicles

It is now well established that under commonly encountered conditions a good approximation to the transient Green’s function G(xa|xb,t) between points xa and xb can be estimated by taking the time derivative of the correlation function Cab(t) of records of ambient noise measured at locations xa and xb. We consider the relationship between Cab(t) and G(xa|xb,t) in a multipathing environment in the geometric limit, and we assume that the noise field has a broad bandwidth. Under these conditions Cab(t) for t > 0 consists of a superposition of signed step functions and two‐sided logarithmic singularities that are delayed in time by the travel times of the rays connecting xa and xb. The reason that Cab has this structure is explained. [Work supported by ONR.]

Noise interferometry, in the geometric limit, in a multipathing environment.

Introduction. e purpose of this study was to evaluate the utilization of spinal thrust manipulation in the management of patients with low back pain (LBP) among physical therapists from New York State (NYS), as well as to evaluate physical therapist knowledge of a lumbar spine manipulation clinical prediction rule (CPR) and whether their NYS physical therapy practice act allows for spinal thrust manipulation to be performed. Materials and Methods. We invited the 300 physical therapy clinics from NYS who serve as clinical instruction sites for the Department of Physical erapy at Daemen College in Amherst, NY, to participate in this survey-based study. One hundred fifty physical therapists completed the survey and were included in the analysis (54% were female and 45.3% were male; 1 respondent did not answer); the mean number of years of physical therapy practice of the participants was 13.36 9.9 years (range, 1–44 years). Participants were invited to complete a survey that was comprised of questions relative to demographics, the use of thrust manipulation in the treatment of patients with LBP, their knowledge of amanipulationCPR, and theNYSphysical therapy practice act and its ability to allow physical therapists to perform thrust manipulation. Chi-square tests, 1-way analyses of variance, and t tests were used for analyses. Results. Of the sample population, 41.3% reported performing spinal thrust manipulation, and the majority of those physical therapists (77.4%) use the intervention between 0% and 25% of the time. irty-seven percent of clinicians who reported manipulating patients with LBP reported using a CPR to determine candidates formanipulation; the remainder of the respondents (63%) did not provide an answer or were unsure. Of the sample population, 63.9% correctly answered the survey question regarding the NYS physical therapy practice act and an ability to legally perform thrust manipulation. Physical therapists who are board certified in orthopedics through the American Physicalerapist Association (P= .005) or residency/fellowship trained in manual physical therapy (P = .03) are significantly more likely to perform thrust manipulation than those who are not. Physical therapists who understand the NYS physical therapy practice act (P = .014), attend continuing education regarding the management of patients with LBP (P = .007), and are male (P < .00001) are also significantly more likely to perform thrust manipulation for patients with LBP. Conclusions. Despite emerging evidence to support the use of thrust manipulation in the management of patients with LBP, utilization of thrust manipulation among physical therapists still remains relatively low. Physical therapists who are board certified in orthopedics and/or residency/ fellowship trained, attend continuing education, and better understand the NYS physical therapy practice act are more likely to perform thrust manipulation.e results of this study may have implications for professional development and educational efforts regarding the training of physical therapists in the utilization of thrust manipulation.

The Utilization of Spinal Thrust Manipulation by Physical Therapists in New York State

The influence of loading rate on pile behaviour in clay

The Kuiper belt object Orcus and its satellite Vanth form an unusual system in the Kuiper belt. Orcus is amongst the largest objects known in the Kuiper belt, but the relative size of Vanth is much larger than that of the tiny satellites of the other large objects. From Hubble Space Telescope observations we find that Orcus and Vanth have different visible colors and that Vanth does not share the water ice absorption feature seen in the infrared spectrum of Orcus. We also find that Vanth has a nearly face-on circular orbit with a period of 9.5393 +-0.0001 days and semimajor axis of 8980+-20 km, implying a system mass of 6.32+- 0.01 X 10^20 kg or 3.8% the mass of dwarf planet Eris. 
From Spitzer Space Telescope observations we find that the thermal emission is consistent with a single body with diameter 940+-70 km and a geometric albedo of 0.28+-0.04. Assuming equal densities and albedos, this measurements implies sizes of Orcus and Vanth of 900 and 280 km, respectively, and a mass ratio of 33. Assuming a factor of 2 lower albedo for the non-icy Vanth, however, implies sizes of 820 and 640 km and a mass ratio of 2. The measured density depends on the assumed albedo ratio of the two objects but is approximately 1.5+-0.3 g cm^-3$, midway between typical densities measured for larger and for smaller objects. The orbit and mass ratio is consistent with formation from a giant impact and subsequent outward tidal evolution and even consistent with the system having now achieved a double synchronous state. The system can equally well be explained, however, by initial eccentric capture, Kozai cycling which increases the eccentricity and decreases the pericenter of the orbit of Vanth, and subsequent tidal evolution inward.

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The size, density, and formation of the Orcus-Vanth system in the Kuiper belt

For an explicit test of the ability to recover the galaxy two-point correlation function from the Lick catalog of Shane and Wirtanen, we have applied the reduction and analysis methods of Seidner et al and Groth and Peebles to model galaxy distributions that have known plate and field "errors" and that are high-fidelity simulations of the Lick sample The model galaxy space distribution is constructed with the Soneira-Peebles prescription, which generates model distributions which have two-, three-, and four-point correlation functions in good agreement with the observed correlation functions The space distribution is projected onto the sky with and without plate "errors" The Seidner et al analysis recovers the plate factors in the former case with an error of 63%, as originally estimated The two-point correlation function estimated from the "corrected" model catalog reproduces the built-in correlation function including the break from the power law This is also true if the angular scale of the break is increased or decreased by a factor of 176 from the observed
value We also compare a map of the corrected counts with a map of the counts projected without plate errors and find that the corrected map is a good visual representation of the galaxy distribution Finally, we construct a simulation which includes systematic variations in plate sensitivity with observer and time-so called "plate shape gradients" Once again, the correlation function of the model catalog reproduces the built in correlation function

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Michael E. Brown

Papers

Noise interferometry, in the geometric limit, in a multipathing environment.

The Utilization of Spinal Thrust Manipulation by Physical Therapists in New York State

The influence of loading rate on pile behaviour in clay

The size, density, and formation of the Orcus-Vanth system in the Kuiper belt

The Shane Wirtanen counts - Observability of the galaxy correlation function