1,848 research outputs found
A social solution to the puzzle of doxastic responsibility: a two-dimensional account of responsibility for belief
In virtue of what are we responsible for our beliefs? I argue that doxastic responsibility has a crucial social component: part of being responsible for our beliefs is being responsible to others. I suggest that this responsibility is a form of answerability with two distinct dimensions: an individual and an interpersonal dimension. While most views hold that the individual dimension is grounded in some form of control that we can exercise over our beliefs, I contend that we are answerable for our beliefs as long as they reflect our evaluative commitments and dispositions, or are products of our reasoning, where this does not amount to a form of control. I next argue that answerability has a second, largely neglected dimension: the interpersonal dimension, which is grounded in what I call our relations of doxastic dependence. As social creatures, we depend on one another in our capacity as believers. We depend on one another as believers not only in epistemic ways, but also in practical ways, because our beliefs inform and motivate our actions, and allow us to participate in shared practical goals. Depending on one another in these ways is an unavoidable part of cooperating in the shared project of pursuing epistemic and practical success, and it makes us vulnerable to both epistemic and moral harm. It is because of this, I argue, that answerability has interpersonal normative force upon us: we are subject to legitimate expectations associated with participating in relations of doxastic dependence
Doxastic responsibility, guidance control, and ownership of belief
ABSTRACTThe contemporary debate over responsibility for belief is divided over the issue of whether such responsibility requires doxastic control, and whether this control must be voluntary in nature. It has recently become popular to hold that responsibility for belief does not require voluntary doxastic control, or perhaps even any form of doxastic ‘control’ at all. However, Miriam McCormick has recently argued that doxastic responsibility does in fact require quasi-voluntary doxastic control: “guidance control,” a complex, compatibilist form of control. In this paper, I pursue a negative and a positive task. First, I argue that grounding doxastic responsibility in guidance control requires too much for agents to be the proper targets for attributions of doxastic responsibility. I will focus my criticisms on three cases in which McCormick's account gives the intuitively wrong verdict. Second, I develop a modified conception of McCormick's notion of “ownership of belief,” which I call Weak Doxastic Ownership. I employ this conception to argue that responsibility for belief is possible even in the absence of guidance control. In doing so, I argue that the notion of doxastic ownership can do important normative work in grounding responsibility for belief without being subsumed under or analyzed in terms of the notion of doxastic control
Comments on ''Wave damping computation for a viscous liquid of finite depth'' by F. Biesel, La Houille Blanche, no. 5, 630-634 /1949/
Validity of wave damping computation for viscous liquid of finite dept
The taxonomic distribution of asteroids from multi-filter all-sky photometric surveys
The distribution of asteroids across the Main Belt has been studied for
decades to understand the compositional distribution and what that tells us
about the formation and evolution of our solar system. All-sky surveys now
provide orders of magnitude more data than targeted surveys. We present a
method to bias-correct the asteroid population observed in the Sloan Digital
Sky Survey (SDSS) according to size, distance, and albedo. We taxonomically
classify this dataset consistent with the Bus and Bus-DeMeo systems and present
the resulting taxonomic distribution. The dataset includes asteroids as small
as 5 km, a factor of three in diameter smaller than in previous works. Because
of the wide range of sizes in our sample, we present the distribution by
number, surface area, volume, and mass whereas previous work was exclusively by
number. While the distribution by number is a useful quantity and has been used
for decades, these additional quantities provide new insights into the
distribution of total material. We find evidence for D-types in the inner main
belt where they are unexpected according to dynamical models of implantation of
bodies from the outer solar system into the inner solar system during planetary
migration (Levison et al. 2009). We find no evidence of S-types or other
unexpected classes among Trojans and Hildas, albeit a bias favoring such a
detection. Finally, we estimate for the first time the total amount of material
of each class in the inner solar system. The main belt's most massive classes
are C, B, P, V and S in decreasing order. Excluding the four most massive
asteroids, Ceres, Pallas, Vesta and Hygiea that heavily skew the values,
primitive material (C-, P-types) account for more than half main-belt and
Trojan asteroids by mass, most of the remaining mass being in the S-types. All
the other classes are minor contributors to the material between Mars and
Jupiter.Comment: Accepted for publication in Icarus -- 43 pages, 15 figures, 7 table
First disk-resolved spectroscopy of (4) Vesta
Vesta, the second largest Main Belt asteroid, will be the first to be
explored in 2011 by NASA's Dawn mission. It is a dry, likely differentiated
body with spectrum suggesting that is has been resurfaced by basaltic lava
flows, not too different from the lunar maria.
Here we present the first disk-resolved spectroscopic observations of an
asteroid from the ground. We observed (4) Vesta with the ESO-VLT adaptive
optics equipped integral-field near-infrared spectrograph SINFONI, as part of
its science verification campaign. The highest spatial resolution of ~90 km on
Vesta's surface was obtained during excellent seeing conditions (0.5") in
October 2004.
We observe spectral variations across Vesta's surface that can be interpreted
as variations of either the pyroxene composition, or the effect of surface
aging. We compare Vesta's 2 micron absorption band to that of
howardite-eucrite-diogenite (HED) meteorites that are thought to originate from
Vesta, and establish particular links between specific regions and HED
subclasses. The overallcomposition is found to be mostly compatible with
howardite meteorites, although a small area around 180 deg. East longitude
could be attributed to a diogenite-rich spot. We finally focus our spectral
analysis on the characteristics of Vesta's bright and dark regions as seen from
Hubble Space Telescope's visible and Keck-II's near-infrared images.Comment: 13 pages, 11 figures, 3 table
Precovery of near-Earth asteroids by a citizen-science project of the Spanish Virtual Observatory
This article describes a citizen-science project conducted by the Spanish
Virtual Observatory (SVO) to improve the orbits of near-Earth asteroids (NEAs)
using data from astronomical archives. The list of NEAs maintained at the Minor
Planet Center (MPC) is checked daily to identify new objects or changes in the
orbital parameters of already catalogued objects. Using NEODyS we compute the
position and magnitude of these objects at the observing epochs of the 938 046
images comprising the Eigth Data Release of the Sloan Digitised Sky Survey
(SDSS). If the object lies within the image boundaries and the magnitude is
brighter than the limiting magnitude, then the associated image is visually
inspected by the project's collaborators (the citizens) to confirm or discard
the presence of the NEA. If confirmed, accurate coordinates and, sometimes,
magnitudes are submitted to the MPC. Using this methodology, 3,226 registered
users have made during the first fifteen months of the project more than
167,000 measurements which have improved the orbital elements of 551 NEAs (6%
of the total number of this type of asteroids). Even more remarkable is the
fact that these results have been obtained at zero cost to telescope time as
NEAs were serendipitously observed while the survey was being carried out. This
demonstrates the enormous scientific potential hidden in astronomical archives.
The great reception of the project as well as the results obtained makes it a
valuable and reliable tool for improving the orbital parameters of near-Earth
asteroids.Comment: 9 pages, 5 figures. Accepted in Astron. Nach
Evidence of a metal-rich surface for the asteroid (16) Psyche from interferometric observations in the thermal infrared
We describe the first determination of thermal properties and size of the
M-type asteroid (16) Psyche from interferometric observations obtained with the
Mid-Infrared Interferometric Instrument (MIDI) of the Very Large Telescope
Interferometer. We used a thermophysical model to interpret our interferometric
data. Our analysis shows that Psyche has a low macroscopic surface roughness.
Using a convex 3-D shape model obtained by Kaasalainen et al. (2002, Icarus
159, 369-395), we derived a volume-equivalent diameter for (16) Psyche of 247
+- 25 km or 238 +- 24 km, depending on the possible values of surface
roughness. Our corresponding thermal inertia estimates are 133 or 114
J.m-2.s-0.5.K-1, with a total uncertainty estimated to 40 J.m-2.s-0.5.K-1. They
are among the highest thermal inertia values ever measured for an asteroid of
this size. We consider this as a new evidence of a metal-rich surface for the
asteroid (16) Psyche.Comment: 45 pages (in referee and preprint format), 6 figure
Spectral properties of near-Earth and Mars-crossing asteroids using Sloan photometry
The nature and origin of the asteroids orbiting in near-Earth space,
including those on a potentially hazardous trajectory, is of both scientific
interest and practical importance. We aim here at determining the taxonomy of a
large sample of near-Earth (NEA) and Mars-crosser (MC) asteroids and analyze
the distribution of these classes with orbit. We use this distribution to
identify their source regions and to study the strength of planetary encounters
to refresh asteroid surfaces. We measure the photometry of these asteroids over
four filters at visible wavelengths on images taken by the SDSS. These colors
are used to classify the asteroids into a taxonomy consistent with the widely
used Bus-DeMeo taxonomy based on spectroscopy. We report here on the taxonomic
classification of 206 NEAs and 776 MCs determined from SDSS photometry,
representing an increase of 40% and 663% of known taxonomy classifications in
these populations. Using the source region mapper by Greenstreet et al. (2012),
we compare the taxonomic distribution among NEAs and main-belt asteroids of
similar diameters. Both distributions agree at the few percent level for the
inner part of the Main Belt and we confirm this region as a main source of
near-Earth objects. The effect of planetary encounters on asteroid surfaces are
also studied by developing a simple model of forces acting on a surface grain
during planetary encounter, which provides the minimum distance at which a
close approach should occur to trigger resurfacing events. By integrating
numerically the orbit of the 519 S-type and 46 Q-type asteroids back in time
and monitoring their encounter distance with planets, we seek to understand the
conditions for resurfacing events. The population of Q-type is found to present
statistically more encounters with Venus and the Earth than S-types, although
both types present the same amount of encounters with Mars.Comment: Accepted for publication in Icarus. 45 pages, 11 figures, 4 tables, 2
tables in appendix (supplementary material
The Micro and Macro of Labor Market Policies
This dissertation documents new evidence on the effects of labor market institutions and provides new tools to assess the impact of labor policies. Many labor market regulations remain controversial, and we lack evidence connecting the impact of these regulations on firms and workers and their aggregate effects. The dissertation evaluates the effects of labor market reforms at the microeconomic level (on workers and firms) and at the aggregate level (on overall employment, welfare, and the unemployment rate). It also accounts for spillovers, general equilibrium effects and heterogeneity to connect the micro and macro impacts. Relying on administrative data on workers and firms and reduced-form evaluation methods, I provide evidence on the effects of labor market policies on targeted individuals and firms, but also on the indirect effects. Second, to quantify the aggregate impact accounting for both direct and indirect effects, I build and estimate structural models, allowing for general equilibrium effects on the labor market. Chapter 1 studies an increase in the level of employment protection in Portugal and Chapter 2 considers the introduction of a minimum working time in France
Prediction of transits of solar system objects in Kepler/K2 images: An extension of the Virtual Observatory service SkyBoT
All the fields of the extended space mission Kepler/K2 are located within the
ecliptic. Many solar system objects thus cross the K2 stellar masks on a
regular basis. We aim at providing to the entire community a simple tool to
search and identify solar system objects serendipitously observed by Kepler.
The SkyBoT service hosted at IMCCE provides a Virtual Observatory (VO)
compliant cone-search that lists all solar system objects present within a
field of view at a given epoch. To generate such a list in a timely manner,
ephemerides are pre-computed, updated weekly, and stored in a relational
database to ensure a fast access. The SkyBoT Web service can now be used with
Kepler. Solar system objects within a small (few arcminutes) field of view are
identified and listed in less than 10 sec. Generating object data for the
entire K2 field of view (14{\deg}) takes about a minute. This extension of the
SkyBot service opens new possibilities with respect to mining K2 data for solar
system science, as well as removing solar system objects from stellar
photometric time-series
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