4,526 research outputs found
Laminin-6 and Laminin-5 Are Recognized by Autoantibodies in a Subset of Cicatricial Pemphigoid
We characterized basement membrane zone (BMZ) autoantigens targeted by autoantibodies (AAb) from patients with cicatricial pemphigoid. Serum from a patient with severe oral cicatricial pemphigoid contained IgG anti-BMZ AAb. The AAb labeled a lower BMZ component on salt-split skin and localized to the lower lamina lucida/lamina densa by direct and indirect immunoelectron microscopy (HEM) but did not label blood vessels. The AAb did not react with EHS laminin-1 and type IV collagen, pepsinized human type IV collagen, recombinant entactin, or NC1 domain of type VII collagen by dot blotting and western blotting. We focused our studies on the laminin family, as laminin-5 was identified as an autoantigen in cicatricial pemphigoid. Culture-conditioned media from normal keratinocytes (containing laminin-6 and laminin-5) and JEB keratinocytes (containing laminin-6 but not laminin-5) were studied by western blotting. Under nonreducing conditions, the patient's AAb recognized a 600-kDa protein (laminin-6) intensely and a 400-kDa protein (laminin-5) weakly in normal keratinocyte medium even though abundant laminin-5 was present. In JEB keratinocyte medium, however, the 600-kDa protein (laminin-6) alone was recognized by the patient's AAb. The AAb also immunolabeled BMZ of JEB skin that lacked laminin-5. The AAb from this patient and two other patients with anti-laminin-5 cicatricial pemphigoid immunoprecipitated both laminin-6 an4 laminin-5. Taken together, the results of IEM, non-reducing western blotting, immunoprecipitation, and JEB skin BMZ immunolabeling indicate that laminin-6, as well as laminin-5, is identified by the AAb from a subset of cicatricial pemphigoid patients. We propose the name âanti-laminin cicatricial pemphigoidâ for this subset
Clusters at Half Hubble Time: Galaxy Structure and Colors in RXJ0152.7-1357 and MS1054-03
We study the photometric and structural properties of spectroscopically
confirmed members in the two massive X-ray--selected z=0.83 galaxy clusters
MS1054-03 and RXJ0152-1357 using three-band mosaic imaging with the Hubble
Space Telescope Advanced Camera for Surveys. The samples include 105 and 140
members of MS1054-03 and RXJ0152-1357, respectively, with ACS F775W magnitude <
24.0. We develop a promising new structural classification method, based on a
combination of the best-fit Sersic indices and the normalized root-mean-square
residuals from the fits; the resulting classes agree well with the visual ones,
but are less affected by galaxy orientation. We examine the color--magnitude
relations in detail and find that the color residuals correlate with the local
mass density measured from our weak lensing maps; we identify a threshold
density of , in units of the critical density, above which
the star formation appears to cease. For RXJ0152-1357, we also find a trend in
the color residuals with velocity, resulting from an offset of about 980 km/s
in the mean redshifts of the early- and late-type galaxies. Analysis of the
color--color diagrams indicates that a range of star formation time-scales are
needed to reproduce the loci of the galaxy colors. We also identify some
cluster galaxies whose colors can only be explained by large amounts, mag, of internal dust extinction. [Abstract shortened]Comment: 30 pages, emulateapj format; 23 figures, many in color. Accepted by
ApJ; scheduled for the 10 June 2006 issue. Some figures degraded; for a
higher resolution version, see: http://astro.wsu.edu/blakeslee/z1clusters
The Morphology - Density Relation in z ~ 1 Clusters
We measure the morphology--density relation (MDR) and morphology-radius
relation (MRR) for galaxies in seven z ~ 1 clusters that have been observed
with the Advanced Camera for Surveys on board the Hubble Space Telescope.
Simulations and independent comparisons of ourvisually derived morphologies
indicate that ACS allows one to distinguish between E, S0, and spiral
morphologies down to zmag = 24, corresponding to L/L* = 0.21 and 0.30 at z =
0.83 and z = 1.24, respectively. We adopt density and radius estimation methods
that match those used at lower redshift in order to study the evolution of the
MDR and MRR. We detect a change in the MDR between 0.8 < z < 1.2 and that
observed at z ~ 0, consistent with recent work -- specifically, the growth in
the bulge-dominated galaxy fraction, f_E+SO, with increasing density proceeds
less rapidly at z ~ 1 than it does at z ~ 0. At z ~ 1 and density <= 500
galaxies/Mpc^2, we find = 0.72 +/- 0.10. At z ~ 0, an E+S0 population
fraction of this magnitude occurs at densities about 5 times smaller. The
evolution in the MDR is confined to densities >= 40 galaxies/Mpc^2 and appears
to be primarily due to a deficit of S0 galaxies and an excess of Spiral+Irr
galaxies relative to the local galaxy population. The Elliptical fraction -
density relation exhibits no significant evolution between z = 1 and z = 0. We
find mild evidence to suggest that the MDR is dependent on the bolometric X-ray
luminosity of the intracluster medium. Implications for the evolution of the
disk galaxy population in dense regions are discussed in the context of these
observations.Comment: 30 pages, 18 figures. Accepted for publication in ApJ. Full
resolution versions of figs 2,3,6,8 are available at
http://www.stsci.edu/~postman/mdr_figure
The Environmental Dependence of Properties of Galaxies around the RDCSJ0910+54 Cluster at z=1.1
(Abridged) We report on the environmental dependence of properties of
galaxies around the RDCSJ0910+54 cluster at z=1.1. We have obtained multi-band
wide-field images of the cluster with Suprime-Cam and MOIRCS on Subaru and
WFCAM on UKIRT. Also, an intensive spectroscopic campaign has been carried out
using LRIS on Keck and FOCAS on Subaru. We discover a possible large-scale
structure around the cluster in the form of three clumps of galaxies. This is
potentially one of the largest structures found so far in the z>1 Universe. We
then examine stellar populations of galaxies in the structure. Red galaxies
have already become the dominant population in the cores of rich clusters at
z~1, and the fraction of red galaxies has not strongly changed since then. The
red fraction depends on richness of clusters in the sense that it is higher in
rich clusters than in poor groups. The luminosity function of red galaxies in
rich clusters is consistent with that in local clusters. On the other hand,
luminosity function of red galaxies in poor groups shows a deficit of faint red
galaxies. This confirms our earlier findings that galaxies follow an
environment-dependent down-sizing evolution. There seems to be a large
variation in the evolutionary phases of galaxies in groups with similar masses.
Further studies of high-z clusters will be a promising way of addressing the
role of nature and nurture effects on galaxy evolution.Comment: 11 pages, 10 figures, accepted for publication in A&
Evolution in the Cluster Early-type Galaxy Size-Surface Brightness Relation at z =~ 1
We investigate the evolution in the distribution of surface brightness, as a
function of size, for elliptical and S0 galaxies in the two clusters RDCS
J1252.9-2927, z=1.237 and RX J0152.7-1357, z=0.837. We use multi-color imaging
with the Advanced Camera for Surveys on the Hubble Space Telescope to determine
these sizes and surface brightnesses. Using three different estimates of the
surface brightnesses, we find that we reliably estimate the surface brightness
for the galaxies in our sample with a scatter of < 0.2 mag and with systematic
shifts of \lesssim 0.05 mag. We construct samples of galaxies with early-type
morphologies in both clusters. For each cluster, we use a magnitude limit in a
band which closely corresponds to the rest-frame B, to magnitude limit of M_B =
-18.8 at z=0, and select only those galaxies within the color-magnitude
sequence of the cluster or by using our spectroscopic redshifts. We measure
evolution in the rest-frame B surface brightness, and find -1.41 \+/- 0.14 mag
from the Coma cluster of galaxies for RDCS J1252.9-2927 and -0.90 \+/- 0.12 mag
of evolution for RX J0152.7-1357, or an average evolution of (-1.13 \+/- 0.15)
z mag. Our statistical errors are dominated by the observed scatter in the
size-surface brightness relation, sigma = 0.42 \+/- 0.05 mag for RX
J0152.7-1357 and sigma = 0.76 \+/- 0.10 mag for RDCS J1252.9-2927. We find no
statistically significant evolution in this scatter, though an increase in the
scatter could be expected. Overall, the pace of luminosity evolution we measure
agrees with that of the Fundamental Plane of early-type galaxies, implying that
the majority of massive early-type galaxies observed at z =~ 1 formed at high
redshifts.Comment: Accepted in ApJ, 16 pages in emulateapj format with 15 eps figures, 6
in colo
The Transformation of Cluster Galaxies at Intermeidate Redshift
We combine imaging data from the Advanced Camera for Surveys (ACS) with
VLT/FORS optical spectroscopy to study the properties of star-forming galaxies
in the z=0.837 cluster CL0152-1357. We have morphological information for 24
star-forming cluster galaxies, which range in morphology from late-type and
irregular to compact early-type galaxies. We find that while most star-forming
galaxies have colors bluer than 1.0, eight are in the red
cluster sequence. Among the star-forming cluster population we find five
compact early-type galaxies which have properties consistent with their
identification as progenitors of dwarf elliptical galaxies. The spatial
distribution of the star-forming cluster members is nonuniform. We find none
within Mpc of the cluster center, which is highly suggestive of an
intracluster medium interaction. We derive star formation rates from [OII]
line fluxes, and use these to compare the global star
formation rate of CL0152-1357 to other clusters at low and intermediate
redshifts. We find a tentative correlation between integrated star formation
rates and , in the sense that hotter clusters have lower integrated star
formation rates. Additional data from clusters with low X-ray temperatures is
needed to confirm this trend. We do not find a significant correlation with
redshift, suggesting that evolution is either weak or absent between z=0.2-0.8.Comment: ApJ accepte
Evolution of the Color-Magnitude Relation in High-Redshift Clusters: Blue Early-Type Galaxies and Red Pairs in RDCS J0910+5422
The color-magnitude relation has been determined for the RDCS J0910+5422
cluster of galaxies at redshift z = 1.106. Cluster members were selected from
HST ACS images, combined with ground--based near--IR imaging and optical
spectroscopy. The observed early--type color--magnitude relation (CMR) in
(i_775 -z_850) versus z_850 shows intrinsic scatters in color of 0.042 +/-
0.010 mag and 0.044 +/- 0.020 mag for ellipticals and S0s, respectively. From
the scatter about the CMR, a mean luminosity--weighted age t > 3.3 Gyr (z > 3)
is derived for the elliptical galaxies.
Strikingly, the S0 galaxies in RDCS J0910+5422 are systematically bluer in
(i_775 - z_850) by 0.07 +/- 0.02 mag, with respect to the ellipticals. The
ellipticity distribution as a function of color indicates that the face-on S0s
in this particular cluster have likely been classified as elliptical. Thus, if
anything, the offset in color between the elliptical and S0 populations may be
even more significant.
The color offset between S0 and E corresponds to an age difference of ~1 Gyr,
for a single-burst solar metallicity model. A solar metallicity model with an
exponential decay in star formation will reproduce the offset for an age of 3.5
Gyr, i.e. the S0s have evolved gradually from star forming progenitors.
The early--type population in this cluster appears to be still forming. The
blue early-type disk galaxies in RDCS J0910+5422 likely represent the direct
progenitors of the more evolved S0s that follow the same red sequence as
ellipticals in other clusters.
Thirteen red galaxy pairs are observed and the galaxies associated in pairs
constitute ~40% of the CMR galaxies in this cluster.Comment: ApJ, in pres
Enzyme-linked immunoassay for dengue virus IgM and IgG antibodies in serum and filter paper blood
BACKGROUND: The reproducibilty of dengue IgM and IgG ELISA was studied in serum and filter paper blood spots from Vietnamese febrile patients. METHODS: 781 pairs of acute (t0) and convalescent sera, obtained after three weeks (t3) and 161 corresponding pairs of filter paper blood spots were tested with ELISA for dengue IgG and IgM. 74 serum pairs were tested again in another laboratory with similar methods, after a mean of 252 days. RESULTS: Cases were classified as no dengue (10 %), past dengue (55%) acute primary (7%) or secondary (28%) dengue. Significant differences between the two laboratories' results were found leading to different diagnostic classification (kappa 0.46, p < 0.001). Filter paper results correlated poorly to serum values, being more variable and lower with a mean (95% CI) difference of 0.82 (0.36 to 1.28) for IgMt3, 0.94 (0.51 to 1.37) for IgGt0 and 0.26 (-0.20 to 0.71) for IgGt3. This also led to differences in diagnostic classification (kappa value 0.44, p < 0.001) The duration of storage of frozen serum and dried filter papers, sealed in nylon bags in an air-conditioned room, had no significant effect on the ELISA results. CONCLUSION: Dengue virus IgG antibodies in serum and filter papers was not affected by duration of storage, but was subject to inter-laboratory variability. Dengue virus IgM antibodies measured in serum reconstituted from blood spots on filter papers were lower than in serum, in particular in the acute phase of disease. Therefore this method limits its value for diagnostic confirmation of individual patients with dengue virus infections. However the detection of dengue virus IgG antibodies eluted from filter paper can be used for sero-prevalence cross sectional studies
Feedback and Brightest Cluster Galaxy Formation: ACS Observations of the Radio Galaxy TN J1338--1942 at z=4.1
We present deep optical imaging of the z=4.1 radio galaxy TN J1338--1942
obtained using the ACS on-board HST. The radio galaxy is known to reside within
a large galaxy overdensity (both in physical extent and density contrast).
There is good evidence that this `protocluster' region is the progenitor of a
present-day rich galaxy cluster. TN J1338 is the dominant galaxy in the
protocluster, in terms of size and luminosity and therefore seems destined to
evolve into the brightest cluster galaxy. The high spatial-resolution ACS
images reveal several kpc-scale features within and around the radio galaxy.
The continuum light is aligned with the radio axis and is resolved into two
clumps in the i-band and z-band bands. These components have luminosities ~10^9
L_sun and sizes of a few kpc. The estimated star-formation rate for the whole
radio galaxy is ~200 M_sun/yr. A simple model in which the jet has triggered
star-formation in these continuum knots is consistent with the available data.
An unusual feature is seen in Lyman-alpha emission. A wedge-shaped extension
emanates from the radio galaxy perpendicularly to the radio axis. This `wedge'
naturally connects to the surrounding, asymmetric, large-scale (~100 kpc)
Lyman-alpha halo. We posit that the wedge is a starburst-driven superwind,
associated with the first major epoch of formation of the brightest cluster
galaxy. The shock and wedge are examples of feedback processes due to both AGN
and star-formation in the earliest stages of massive galaxy formation.Comment: 41 pages, 12 figures. Accepted to Ap
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PGC1α-dependent NAD biosynthesis links oxidative metabolism to renal protection
The energetic burden of continuously concentrating solutes against gradients along the tubule may render the kidney especially vulnerable to ischemia. Indeed, acute kidney injury (AKI) affects 3% of all hospitalized patients.1,2 Here we show that the mitochondrial biogenesis regulator, PGC1α,3,4 is a pivotal determinant of renal recovery from injury by regulating NAD biosynthesis. Following renal ischemia, PGC1αâ/â mice developed local deficiency of the NAD precursor niacinamide (Nam), marked fat accumulation, and failure to re-establish normal function. Remarkably, exogenous Nam improved local NAD levels, fat accumulation, and renal function in post-ischemic PGC1αâ/â mice. Inducible tubular transgenic mice (iNephPGC1α) recapitulated the effects of Nam supplementation, including more local NAD and less fat accumulation with better renal function after ischemia. PGC1α coordinately upregulated the enzymes that synthesize NAD de novo from amino acids whereas PGC1α deficiency or AKI attenuated the de novo pathway. Nam enhanced NAD via the enzyme NAMPT and augmented production of the fat breakdown product beta-hydroxybutyrate (ÎČ-OHB), leading to increased prostaglandin PGE2, a secreted autocoid that maintains renal function.5 Nam treatment reversed established ischemic AKI and also prevented AKI in an unrelated toxic model. Inhibition of ÎČ-OHB signaling or prostaglandins similarly abolished PGC1α-dependent renoprotection. Given the importance of mitochondrial health in aging and the function of metabolically active organs, the results implicate Nam and NAD as key effectors for achieving PGC1α-dependent stress resistance
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