579 research outputs found
X-Ray Wakes in Abell 160
`Wakes' of X-ray emission have now been detected trailing behind a few (at
least seven) elliptical galaxies in clusters. To quantify how widespread this
phenomenon is, and what its nature might be, we have obtained a deep (70 ksec)
X-ray image of the poor cluster Abell 160 using the ROSAT HRI. Combining the
X-ray data with optical positions of confirmed cluster members, and applying a
statistic designed to search for wake-like excesses, we confirm that this
phenomenon is observed in galaxies in this cluster. The probability that the
detections arise from chance is less than 0.0038. Further, the wakes are not
randomly distributed in direction, but are preferentially oriented pointing
away from the cluster centre. This arrangement can be explained by a simple
model in which wakes arise from the stripping of their host galaxies'
interstellar media due to ram pressure against the intracluster medium through
which they travel.Comment: 7 pages, 7 figures, accepted for publication in MNRA
Behavior of steel building connections subjected to inelastic strain reversals
Inelastic design of steel structures to withstand seismic forces requires a knowledge of the behavior of connections when subjected to cyclically reversed loading. This report contains a description of the design and testing of selected steel beam-to-column connection specimens. The motivations for the choice of connection types and overall geometry of the specimens are discussed, relating them to full-size prototypes used in actual building frames. The characteristics of the test installation are described, including means of loading, type of lateral support provided, etc. The programs of cycling of all tests are presented in terms of the deflection of the tip of the cantilever beam. Typical hysteresis diagrams and failure photographs are also included. The outstanding features of the behavior of several specimens during testing are discussed and compared, and possible explanations given for particular aspects. Finally, the results of all of the tests are summarized, and an attempt made to draw comparisons and conclusions of somewhat broader applicability
Behavior of steel building connections subjected to inelastic strain reversals experimental data
Reflowable documents composed from pre-rendered atomic components
Mobile eBook readers are now commonplace in today’s society, but their document layout algorithms remain basic, largely due to constraints imposed by short battery life. At present, with any eBook file format not based on PDF, the layout of the document, as it appears to the end user, is at the mercy of hidden reformatting and reflow algorithms interacting with the screen parameters of the device on which the document is rendered. Very little control is provided to the publisher or author, beyond some basic formatting options.
This paper describes a method of producing well-typeset, scalable, document layouts by embedding several pre-rendered versions of a document within one file, thus enabling many computationally expensive steps (e.g. hyphenation and line-breaking) to be carried out at document compilation time, rather than at ‘view time’. This system has the advantage that end users are not constrained to a single, arbitrarily chosen view of the document, nor are they subjected to reading a poorly typeset version rendered on the fly. Instead, the device can choose a layout appropriate to its screen size and the end user’s choice of zoom level, and the author and publisher can have fine-grained control over all layouts
Admission Decision-Making in Hospital Emergency Departments: the Role of the Accompanying Person
In resource-stretched emergency departments, people accompanying patients play key roles in patients' care. This article presents analysis of the ways health professionals and accompanying persons talked about admission decisions and caring roles. The authors used ethnographic case study design involving participant observation and semi-structured interviews with 13 patients, 17 accompanying persons and 26 healthcare professionals in four National Health Service hospitals in south-west England. Focused analysis of interactional data revealed that professionals’ standardization of the patient-carer relationship contrasted with accompanying persons' varied connections with patients. Accompanying persons could directly or obliquely express willingness, ambivalence and resistance to supporting patients’ care. The drive to avoid admissions can lead health professionals to deploy conversational skills to enlist accompanying persons for discharge care without exploring the meanings of their particular relations with patients. Taking a relationship-centered approach could improve attention to accompanying persons as co-producers of healthcare and participants in decision-making
Substructure in clusters containing wide-angle tailed radio galaxies. I. New redshifts
We present new redshifts and positions for 635 galaxies in nine rich clusters
containing Wide-Angle Tailed (WAT) radio galaxies. Combined with existing data,
we now have a sample of 18 WAT-containing clusters with more than 10 redshifts.
This sample contains a substantial portion of the WAT clusters in the VLA 20 cm
survey of Abell clusters, including 75% of WAT clusters in the complete survey
(z0.09. It is a representative sample
which should not contain biases other than selection by radio morphology. We
graphically present the new data using histograms and sky maps. A
semi-automated procedure is used to search for emission lines in the spectra in
order to add and verify galaxy redshifts. We find that the average apparent
fraction of emission line galaxies is about 9% in both the clusters and the
field. We investigate the magnitude completeness of our redshift surveys with
CCD data for a test case, Abell 690. This case indicates that our galaxy target
lists are deeper than the detection limit of a typical MX exposure, and they
are 82% complete down to R=19.0. The importance of the uniformity of the
placement of fibers on targets is posited, and we evaluate this in our
datasets. We find some cases of non-uniformities which may influence dynamical
analyses. A second paper will use this database to look for correlations
between the WAT radio morphology and the cluster's dynamical state.Comment: 15 pages, 5 figures, 7 tables. To appear in the Astronomical Journa
The Black Hole Mass and Extreme Orbital Structure in NGC1399
The largest galaxies, and in particular central galaxies in clusters, offer
unique insight into understanding the mechanism for the growth of nuclear black
holes. We present Hubble Space Telescope kinematics for NGC1399, the central
galaxy in Fornax. We find the best-fit model contains a black hole of 5.1 +-0.7
x 10^8 Msun (at a distance of 21.1 Mpc), a factor of over 2 below the
correlation of black hole mass and velocity dispersion. We also find a dramatic
signature for central tangential anisotropy. The velocity profiles on adjacent
sides 0.5" away from the nucleus show strong bimodality, and the central
spectrum shows a large drop in the dispersion. Both of these observations point
to an orbital distribution that is tangentially biased. The best-fit orbital
model suggests a ratio of the tangential to radial internal velocity
dispersions of three. This ratio is the largest seen in any galaxy to date and
will provide an important measure for the mode by which the central black hole
has grown.Comment: 9 pages, accepted for publication in the Astrophysical Journa
The counterrotating core and the black hole mass of IC1459
The E3 giant elliptical galaxy IC1459 is the prototypical galaxy with a fast
counterrotating stellar core. We obtained one HST/STIS long-slit spectrum along
the major axis of this galaxy and CTIO spectra along five position angles. We
present self-consistent three-integral axisymmetric models of the stellar
kinematics, obtained with Schwarzschild's numerical orbit superposition method.
We study the dynamics of the kinematically decoupled core (KDC) in IC1459 and
we find it consists of stars that are well-separated from the rest of the
galaxy in phase space. The stars in the KDC counterrotate in a disk on orbits
that are close to circular. We estimate that the KDC mass is ~0.5% of the total
galaxy mass or ~3*10^9 Msun. We estimate the central black hole mass M_BH of
IC1459 independently from both its stellar and its gaseous kinematics. Some
complications probably explain why we find rather discrepant BH masses with the
different methods. The stellar kinematics suggest that M_BH = (2.6 +/-
1.1)*10^9 Msun (3 sigma error). The gas kinematics suggests that M_BH ~
3.5*10^8 Msun if the gas is assumed to rotate at the circular velocity in a
thin disk. If the observed velocity dispersion of the gas is assumed to be
gravitational, then M_BH could be as high as ~1.0*10^9 Msun. These different
estimates bracket the value M_BH = (1.1 +/- 0.3)*10^9 Msun predicted by the
M_BH-sigma relation. It will be an important goal for future studies to assess
the reliability of black hole mass determinations with either technique. This
is essential if one wants to interpret the correlation between the BH mass and
other global galaxy parameters (e.g. velocity dispersion) and in particular the
scatter in these correlations (believed to be only ~0.3 dex). [Abridged]Comment: 51 pages, LaTeX with 19 PostScript figures. Revised version, with
three new figures and data tables. To appear in The Astrophysical Journal,
578, 2002 October 2
A Quintet Of Black Hole Mass Determinations
We report five new measurements of central black hole masses based on Space Telescope Imaging Spectrograph and Wide Field Planetary Camera 2 observations with the Hubble Space Telescope (HST) and on axisymmetric, three-integral, Schwarzschild orbit-library kinematic models. We selected a sample of galaxies within a narrow range in velocity dispersion that cover a range of galaxy parameters (including Hubble type and core/power-law surface density profile) where we expected to be able to resolve the galaxy's sphere of influence based on the predicted value of the black hole mass from the M-sigma relation. We find masses for the following galaxies: NGC3585, M(BH) = 3.4(-0.6)(+1.5) x 10(8) M(circle dot;) NGC 3607, M(BH) = 1.2(-0.4)(+0.4) x 10(8) M(circle dot); NGC 4026, M(BH) = 2.1(-0.4)(+0.7) x 10(8) M(circle dot); and NGC 5576, M(BH) = 1.8(-0.4)(+0.3) x 10(8) M(circle dot), all significantly excluding M(BH) = 0. For NGC 3945, M(BH) = 9(-21)(+17) x 10(6) M(circle dot), which is significantly below predictions from M-sigma and M-L relations and consistent with MBH = 0, though the presence of a double bar in this galaxy may present problems for our axisymmetric code.NASA/HST GO-5999, GO-6587, GO-6633, GO-7468, GO-9107NASA NAS 5-26555Astronom
A Stellar Dynamical Measurement of the Black Hole Mass in the Maser Galaxy NGC 4258
We determine the mass of the black hole at the center of the spiral galaxy
NGC 4258 by constructing axisymmetric dynamical models of the galaxy. These
models are constrained by high spatial resolution imaging and long-slit
spectroscopy of the nuclear region obtained with the {\em Hubble Space
Telescope}, complemented by ground-based observations extending to larger
radii. Our best mass estimate is \MBH = (3.3 \pm 0.2) \times 10^7 \MSun for
a distance of 7.28 Mpc (statistical errors only). This is within 15% of
(3.82\pm 0.01) \times 10^7 \MSun, the mass determined from the kinematics of
water masers (rescaled to the same distance) assuming they are in Keplerian
rotation in a warped disk. The construction of accurate dynamical models of NGC
4258 is somewhat compromised by an unresolved active nucleus and color
gradients, the latter caused by variations in the stellar population and/or
obscuring dust. These problems are not present in the other black
hole mass determinations from stellar dynamics that have been published by us
and other groups; thus, the relatively close agreement between the stellar
dynamical mass and the maser mass in NGC 4258 enhances our confidence in the
black hole masses determined in other galaxies from stellar dynamics using
similar methods and data of comparable quality.Comment: 58 pages, submitted to ApJ. Some figures excluded due to size. The
entire paper is at http://www.noao.edu/noao/staff/lauer/nuker_papers.htm
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