1,190 research outputs found
Reionization Constraints on the Contribution of Primordial Compact Objects to Dark Matter
Many lines of evidence suggest that nonbaryonic dark matter constitutes
roughly 30% of the critical closure density, but the composition of this dark
matter is unknown. One class of candidates for the dark matter is compact
objects formed in the early universe, with typical masses M between 0.1 and 1
solar masses to correspond to the mass scale of objects found with microlensing
observing projects. Specific candidates of this type include black holes formed
at the epoch of the QCD phase transition, quark stars, and boson stars. Here we
show that accretion onto these objects produces substantial ionization in the
early universe, with an optical depth to Thomson scattering out to z=1100 of
approximately tau=2-4 [f_CO\epsilon_{-1}(M/Msun)]^{1/2} (H_0/65)^{-1}, where
\epsilon_{-1} is the accretion efficiency \epsilon\equiv L/{\dot M}c^2 divided
by 0.1 and f_CO is the fraction of matter in the compact objects. The current
upper limit to the scattering optical depth, based on the anisotropy of the
microwave background, is approximately 0.4. Therefore, if accretion onto these
objects is relatively efficient, they cannot be the main component of
nonbaryonic dark matter.Comment: 12 pages including one figure, uses aaspp4, submitted to Ap
Deprojection of Rich Cluster Images
We consider a general method of deprojecting 2D images to reconstruct the 3D
structure of the projected object, assuming axial symmetry. The method consists
of the application of the Fourier Slice Theorem to the general case where the
axis of symmetry is not necessarily perpendicular to the line of sight, and is
based on an extrapolation of the image Fourier transform into the so-called
cone of ignorance. The method is specifically designed for the deprojection of
X-ray, Sunyaev-Zeldovich (SZ) and gravitational lensing maps of rich clusters
of galaxies. For known values of the Hubble constant, H0, and inclination
angle, the quality of the projection depends on how exact is the extrapolation
in the cone of ignorance. In the case where the axis of symmetry is
perpendicular to the line of sight and the image is noise-free, the
deprojection is exact. Given an assumed value of H0, the inclination angle can
be found by matching the deprojected structure out of two different images of a
given cluster, e.g., SZ and X-ray maps. However, this solution is degenerate
with respect to its dependence on the assumed H0, and a third independent image
of the given cluster is needed to determine H0 as well. The application of the
deprojection algorithm to upcoming SZ, X-ray and weak lensing projected mass
images of clusters will serve to determine the structure of rich clusters, the
value of H0, and place constraints on the physics of the intra-cluster gas and
its relation to the total mass distribution.Comment: 7 pages, LaTeX, 2 Postscript figures, uses as2pp4.sty. Accepted for
publication in ApJ Letters. Also available at:
http://astro.berkeley.edu:80/~squires/papers/deproj.ps.g
Dark baryons and rotation curves
The best measured rotation curve for any galaxy is that of the dwarf
spiralXXXX DDO 154, which extends out to about 20 disk scale lengths. It
provides an ideal laboratory for testing the universal density profile
prediction from high resolution numerical simulations of hierarchical
clustering in cold dark matter dominated cosmological models. We find that the
observed rotation curve cannot be fit either at small radii, as previously
noted, or at large radii. We advocate a resolution of this dilemma by
postulating the existence of a dark spheroid of baryons amounting to several
times the mass of the observed disk component and comparable to that of the
cold dark matter halo component. Such an additional mass component provides an
excellent fit to the rotation curve provided that the outer halo is still cold
dark matter-dominated with a density profile and mass-radius scaling relation
as predicted by standard CDM-dominated models. The universal existence of such
dark baryonic spheroidal components provides a natural explanation of the
universal rotation curves observed in spiral galaxies, may have a similar
origin and composition to the local counterpart that has been detected as
MACHOs in our own galactic halo via gravitational microlensing, and is
consistent with, and even motivated by, primordial nucleosynthesis estimates of
the baryon fraction.Comment: 16 pages LaTeX, 2 postscript figures. To be published in The
Astrophysical Journal, Letter
Evaluational adjectives
This paper demarcates a theoretically interesting class of "evaluational adjectives." This class includes predicates expressing various kinds of normative and epistemic evaluation, such as predicates of personal taste, aesthetic adjectives, moral adjectives, and epistemic adjectives, among others. Evaluational adjectives are distinguished, empirically, in exhibiting phenomena such as discourse-oriented use, felicitous embedding under the attitude verb `find', and sorites-susceptibility in the comparative form. A unified degree-based semantics is developed: What distinguishes evaluational adjectives, semantically, is that they denote context-dependent measure functions ("evaluational perspectives")—context-dependent mappings to degrees of taste, beauty, probability, etc., depending on the adjective. This perspective-sensitivity characterizing the class of evaluational adjectives cannot be assimilated to vagueness, sensitivity to an experiencer argument, or multidimensionality; and it cannot be demarcated in terms of pretheoretic notions of subjectivity, common in the literature. I propose that certain diagnostics for "subjective" expressions be analyzed instead in terms of a precisely specified kind of discourse-oriented use of context-sensitive language. I close by applying the account to `find x PRED' ascriptions
GMOS Spectroscopy of SCUBA Galaxies Behind A851
We have identified counterparts to two submillimeter (submm) sources, SMM
J09429+4659 and SMM J09431+4700, seen through the core of the z=0.41 cluster
Abell 851. We employ deep 1.4-GHz observations and the far-infrared/radio
correlation to refine the submm positions and then optical and near-infrared
imaging to locate their counterparts. We identify an extremely red counterpart
to SMM J09429+4659, while GMOS spectroscopy with Gemini-North shows that the
R=23.8 radio source identified with SMM J09431+4700 is a hyperluminous infrared
galaxy (L_FIR~1.5x10^13 L_sun) at z=3.35, the highest spectroscopic redshift so
far for a galaxy discovered in the submm. The emission line properties of this
galaxy are characteristic of a narrow-line Seyfert-1, although the lack of
detected X-ray emission in a deep XMM-Newton observation suggests that the bulk
of the luminosity of this galaxy is derived from massive star formation. We
suggest that active nuclei, and the outflows they engender, may be an important
part of the evolution of the brightest submm galaxies at high redshifts.Comment: to appear in the Oct 1 issue of ApJ Letter
The Black Hole Mass - Galaxy Bulge Relationship for QSOs in the SDSS DR3
We investigate the relationship between black hole mass and host galaxy
velocity dispersion for QSOs in Data Release 3 of the Sloan Digital Sky Survey.
We derive black hole mass from the broad Hbeta line width and continuum
luminosity, and the bulge stellar velocity dispersion from the [OIII] narrow
line width. At higher redshifts, we use MgII and [OII] in place of Hbeta and
[OIII]. For redshifts z < 0.5, our results agree with the black hole mass -
bulge velocity dispersion relationship for nearby galaxies. For 0.5 < z < 1.2,
this relationship appears to show evolution with redshift in the sense that the
bulges are too small for their black holes. However, we find that part of this
apparent trend can be attributed to observational biases, including a Malmquist
bias involving the QSO luminosity. Accounting for these biases, we find ~0.2
dex evolution in the black hole mass-bulge velocity dispersion relationship
between now and redshift z ~ 1.Comment: Accepted by ApJ, 15 pages, 9 figure
Early Growth and Efficient Accretion of Massive Black Holes at High Redshift
Black-hole masses of the highest redshift quasars (4 <~ z <~ 6) are estimated
using a previously presented scaling relationship, derived from reverberation
mapping of nearby quasars, and compared to quasars at lower redshift. It is
shown that the central black holes in luminous z >~ 4 quasars are very massive
(>~ 10^9 solar masses). It is argued that the mass estimates of the high-z
quasars are not subject to larger uncertainties than those for nearby quasars.
Specifically, the large masses are not overestimates and the lack of similarly
large black-hole masses in the nearby Universe does not rule out their
existence at high-z. However, AGN host galaxies do not typically appear fully
formed or evolved at these early epochs. This supports scenarios in which black
holes build up mass very fast in a radiatively inefficient (or obscured) phase
relative to the stars in their galaxies. Additionally, upper envelopes of
black-hole mass of approximately 10^{10} solar masses and bolometric luminosity
of ~ 10^{48} erg/s are observed at all redshifts.Comment: 17 pages including 7 figures (5 in color) and 1 table. To appear in
ApJ, v600, January 1, 200
Probing spin-charge separation in a Tomonaga-Luttinger liquid
In a one-dimensional (1D) system of interacting electrons, excitations of
spin and charge travel at different speeds, according to the theory of a
Tomonaga-Luttinger Liquid (TLL) at low energies. However, the clear observation
of this spin-charge separation is an ongoing challenge experimentally. We have
fabricated an electrostatically-gated 1D system in which we observe spin-charge
separation and also the predicted power-law suppression of tunnelling into the
1D system. The spin-charge separation persists even beyond the low-energy
regime where the TLL approximation should hold. TLL effects should therefore
also be important in similar, but shorter, electrostatically gated wires, where
interaction effects are being studied extensively worldwide.Comment: 11 pages, 4 PDF figures, uses scicite.sty, Science.bs
Ribbons on the CBR Sky: A Powerful Test of a Baryon Symmetric Universe
If the Universe consists of domains of matter and antimatter, annihilations
at domain interfaces leave a distinctive imprint on the Cosmic Background
Radiation (CBR) sky. The signature is anisotropies in the form of long, thin
ribbons of width , separated by angle where L is the characteristic domain size, and
y-distortion parameter . Such a pattern could potentially be
detected by the high-resolution CBR anisotropy experiments planned for the next
decade, and such experiments may finally settle the question of whether or not
our Hubble volume is baryon symmetric.Comment: LaTeX, 10 pages, 4 figures in epsf. Revised version corrects a couple
of relevant mistake
Positrons from particle dark-matter annihilation in the Galactic halo: propagation Green's functions
We have made a calculation of the propagation of positrons from dark-matter
particle annihilation in the Galactic halo in different models of the dark
matter halo distribution using our 3D code, and present fits to our numerical
propagation Green's functions. We show that the Green's functions are not very
sensitive to the dark matter distribution for the same local dark matter energy
density. We compare our predictions with computed cosmic ray positron spectra
(``background'') for the ``conventional'' CR nucleon spectrum which matches the
local measurements, and a modified spectrum which respects the limits imposed
by measurements of diffuse Galactic gamma-rays, antiprotons, and positrons. We
conclude that significant detection of a dark matter signal requires favourable
conditions and precise measurements unless the dark matter is clumpy which
would produce a stronger signal. Although our conclusion qualitatively agrees
with that of previous authors, it is based on a more realistic model of
particle propagation and thus reduces the scope for future speculations.
Reliable background evaluation requires new accurate positron measurements and
further developments in modelling production and propagation of cosmic ray
species in the Galaxy.Comment: 8 pages, 6 ps-figures, 3 tables, uses revtex. Accepted for
publication in Physical Review D. More details can be found at
http://www.gamma.mpe-garching.mpg.de/~aws/aws.htm
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