Context.
The hydrogen Lyman
α
line is often the only measurable feature in optical spectra of high-redshift galaxies. Its shape and strength are influenced by radiative transfer processes and the ...properties of the underlying stellar population. High equivalent widths of several hundred Å are especially hard to explain by models and could point towards unusual stellar populations, for example with low metallicities, young stellar ages, and a top-heavy initial mass function. Other aspects influencing equivalent widths are the morphology of the galaxy and its gas properties.
Aims.
The aim of this study is to better understand the connection between the Lyman
α
rest-frame equivalent width (EW
0
) and spectral properties as well as ultraviolet (UV) continuum morphology by obtaining reliable EW
0
histograms for a statistical sample of galaxies and by assessing the fraction of objects with large equivalent widths.
Methods.
We used integral field spectroscopy from the Multi Unit Spectroscopic Explorer (MUSE) combined with broad-band data from the
Hubble
Space Telescope (HST) to measure EW
0
. We analysed the emission lines of 1920 Lyman
α
emitters (LAEs) detected in the full MUSE-Wide (one hour exposure time) and MUSE-Deep (ten hour exposure time) surveys and found UV continuum counterparts in archival HST data. We fitted the UV continuum photometric images using the
Galfit
software to gain morphological information on the rest-UV emission and fitted the spectra obtained from MUSE to determine the double peak fraction, asymmetry, full-width at half maximum, and flux of the Lyman
α
line.
Results.
The two surveys show different histograms of Lyman
α
EW
0
. In MUSE-Wide, 20% of objects have EW
0
> 240 Å, while this fraction is only 11% in MUSE-Deep and ≈16% for the full sample. This includes objects without HST continuum counterparts (one-third of our sample), for which we give lower limits for EW
0
. The object with the highest securely measured EW
0
has EW
0
= 589 ± 193 Å (the highest lower limit being EW
0
= 4464 Å). We investigate the connection between EW
0
and Lyman
α
spectral or UV continuum morphological properties.
Conclusions.
The survey depth has to be taken into account when studying EW
0
distributions. We find that in general, high EW
0
objects can have a wide range of spectral and UV morphological properties, which might reflect that the underlying causes for high EW
0
values are equally varied.
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ABSTRACT We present the first year of Hubble Space Telescope imaging of the unique supernova (SN) "Refsdal," a gravitationally lensed SN at z = 1.488 0.001 with multiple images behind the galaxy ...cluster MACS J1149.6+2223. The first four observed images of SN Refsdal (images S1-S4) exhibited a slow rise (over ∼150 days) to reach a broad peak brightness around 2015 April 20. Using a set of light curve templates constructed from SN 1987A-like peculiar Type II SNe, we measure time delays for the four images relative to S1 of 4 4 (for S2), 2 5 (S3), and 24 7 days (S4). The measured magnification ratios relative to S1 are 1.15 0.05 (S2), 1.01 0.04 (S3), and 0.34 0.02 (S4). None of the template light curves fully captures the photometric behavior of SN Refsdal, so we also derive complementary measurements for these parameters using polynomials to represent the intrinsic light curve shape. These more flexible fits deliver fully consistent time delays of 7 2 (S2), 0.6 3 (S3), and 27 8 days (S4). The lensing magnification ratios are similarly consistent, measured as 1.17 0.02 (S2), 1.00 0.01 (S3), and 0.38 0.02 (S4). We compare these measurements against published predictions from lens models, and find that the majority of model predictions are in very good agreement with our measurements. Finally, we discuss avenues for future improvement of time delay measurements-both for SN Refsdal and for other strongly lensed SNe yet to come.
Summary
Background
Antilaminin 332 mucous membrane pemphigoid (MMP) is an autoimmune subepidermal blistering disease with predominant mucosal involvement and autoantibodies against laminin 332. ...Malignancies have been associated with this disease; however, no standardized detection system for antilaminin 332 serum antibodies is widely available.
Objectives
Development of a sensitive and specific assay for the detection of antilaminin 332 antibodies.
Methods
An indirect immunofluorescence (IF) assay using recombinant laminin 332 was developed and probed with a large number of antilaminin 332 MMP patient sera (n = 93), as well as sera from patients with antilaminin 332‐negative MMP (n = 153), bullous pemphigoid (n = 20), pemphigus vulgaris (n = 20) and noninflammatory dermatoses (n = 22), and healthy blood donors (n = 100).
Results
In the novel IF assay, sensitivities with the laminin 332 heterotrimer and the individual α3, β3 and γ2 chains were 77%, 43%, 41% and 13%, respectively, with specificities of 100% for each substrate. The sensitivity for the heterotrimer increased when an anti‐IgG4 enriched antitotal IgG conjugate was applied. Antilaminin 332 reactivity paralleled disease activity and was associated with malignancies in 25% of patients with antilaminin 332 MMP.
Conclusions
The novel IF‐based assay will facilitate the serological diagnosis of antilaminin 332 MMP and may help to identify patients at risk of a malignancy.
What's already known about this topic?
Antilaminin 332 mucous membrane pemphigoid (MMP) is an autoimmune subepidermal blistering disease with predominant mucosal involvement characterized by antilaminin 332 autoantibodies.
Malignancies have been associated with this disease, but currently no standardized detection system for antilaminin 332 serum antibodies is widely available.
What does this study add?
A sensitive and highly specific immunofluorescence assay for the detection of antilaminin 332 autoantibodies using recombinant laminin 332‐expressing human cells was developed, which will soon be widely available.
What is the translational message?
This assay may not only facilitate the diagnosis of antilaminin 332 MMP but may also be valuable to monitor disease activity and identify patients at risk of a malignancy.
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BFBNIB, FZAB, GIS, IJS, KILJ, NLZOH, NUK, OILJ, SAZU, SBCE, SBMB, UL, UM, UPUK
Rest-frame ultraviolet (UV) emission lines probe electron densities, gas-phase abundances, metallicities, and ionization parameters of the emitting star-forming galaxies and their environments. The ...strongest main UV emission line, Ly
α
, has been instrumental in advancing the general knowledge of galaxy formation in the early universe. However, observing Ly
α
emission becomes increasingly challenging at
z
≳ 6 when the neutral hydrogen fraction of the circumgalactic and intergalactic media increases. Secondary weaker UV emission lines provide important alternative methods for studying galaxy properties at high redshift. We present a large sample of rest-frame UV emission line sources at intermediate redshift for calibrating and exploring the connection between secondary UV lines and the emitting galaxies’ physical properties and their Ly
α
emission. The sample of 2052 emission line sources with 1.5 <
z
< 6.4 was collected from integral field data from the MUSE-Wide and MUSE-Deep surveys taken as part of Guaranteed Time Observations. The objects were selected through untargeted source detection (i.e., no preselection of sources as in dedicated spectroscopic campaigns) in the three-dimensional MUSE data cubes. We searched optimally extracted one-dimensional spectra of the full sample for UV emission features via emission line template matching, resulting in a sample of more than 100 rest-frame UV emission line detections. We show that the detection efficiency of (non-Ly
α
) UV emission lines increases with survey depth, and that the emission line strength of He
II
λ
1640 Å, O
III
λ
1661 + O
III
λ
1666, and Si
III
λ
1883 + Si
III
λ
1892 correlate with the strength of C
III
λ
1907 + C
III
λ
1909. The rest-frame equivalent width (EW
0
) of C
III
λ
1907 + C
III
λ
1909 is found to be roughly 0.22 ± 0.18 of EW
0
(Ly
α
). We measured the velocity offsets of resonant emission lines with respect to systemic tracers. For C
IV
λ
1548 + C
IV
λ
1551 we find that Δ
v
C
IV
≲ 250 km s
−1
, whereas Δ
v
Ly
α
falls in the range of 250−500 km s
−1
which is in agreement with previous results from the literature. The electron density
n
e
measured from Si
III
λ
1883 + Si
III
λ
1892 and C
III
λ
1907 + C
III
λ
1909 line flux ratios is generally < 10
5
cm
−3
and the gas-phase abundance is below solar at 12 + log
10
(O/H)≈8. Lastly, we used “PhotoIonization Model Probability Density Functions” to infer physical parameters of the full sample and individual systems based on photoionization model parameter grids and observational constraints from our UV emission line searches. This reveals that the UV line emitters generally have ionization parameter log
10
(U) ≈ −2.5 and metal mass fractions that scatter around
Z
≈ 10
−2
, that is
Z
≈ 0.66
Z
⊙
. Value-added catalogs of the full sample of MUSE objects studied in this work and a collection of UV line emitters from the literature are provided with this paper.
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A new synthetic platform for the spatially controlled functionalization of phase separated block copolymer nanoparticles is presented. Selective incorporation of chemical functionalities into ...specific domains of striped ellipsoidal nanoparticles is achieved by blending a structure-inducing PS- b -P2VP block copolymer with functionalized PS- co -X and P2VP- co -X copolymers. During self-assembly, the BCP phases incorporate the corresponding functional copolymers which results in their chemical modification without losing control over particle shape and morphology. It was shown that the introduction of benzophenones as photocrosslinking groups allows the preparation of particles which demonstrated a reversible shape change due to triggered swelling/deswelling. This dynamic behavior could be combined with the selective introduction of other moieties such as ferrocene groups or reactive pentafluorostyrene moieties. Ultimately, such combinations opened up new opportunities for post-assembly functionalizations to realize multifunctional particles containing for example ferrocene moieties in the PS domains and Au nanoparticles in the P2VP phase. Overall, a versatile toolbox was developed that enables the formation of tailor-made functional shape anisotropic nanoparticles.
Abstract
We analyse a sample of eight highly magnified galaxies at redshift 0.6 < z < 1.5 observed with MUSE, exploring the resolved properties of these galaxies at sub-kiloparsec scales. Combining ...multiband HST photometry and MUSE spectra, we derive the stellar mass, global star formation rates (SFRs), extinction and metallicity from multiple nebular lines, concluding that our sample is representative of z ∼ 1 star-forming galaxies. We derive the 2D kinematics of these galaxies from the O ii emission and model it with a new method that accounts for lensing effects and fits multiple images simultaneously. We use these models to calculate the 2D beam-smearing correction and derive intrinsic velocity dispersion maps. We find them to be fairly homogeneous, with relatively constant velocity dispersions between 15 and 80 km s−1 and Gini coefficient of ${\lesssim }0.3$. We do not find any evidence for higher (or lower) velocity dispersions at the positions of bright star-forming clumps. We derive resolved maps of dust attenuation and attenuation-corrected SFRs from emission lines for two objects in the sample. We use this information to study the relation between resolved SFR and velocity dispersion. We find that these quantities are not correlated, and the high-velocity dispersions found for relatively low star-forming densities seems to indicate that, at sub-kiloparsec scales, turbulence in high-z discs is mainly dominated by gravitational instability rather than stellar feedback.
ABSTRACT The Wide Field Camera 3 (WFC3) on the Hubble Space Telescope (HST) enabled the search for the first galaxies observed at z ∼ 8-11 (500-700 Myr after the Big Bang). To continue quantifying ...the number density of the most luminous galaxies (MAB ∼ −22.0) at the earliest epoch observable with HST, we search for z ∼ 10 galaxies (F125W-dropouts) in archival data from the Brightest of Reionizing Galaxies (BoRGz8) survey, originally designed for detection of z ∼ 8 galaxies (F098M-dropouts). By focusing on the deepest 293 arcmin2 of the data along 62 independent lines of sight, we identify six z ∼ 10 candidates satisfying the color selection criteria, detected at S/N > 8 in F160W with MAB = −22.8 to −21.1 if at z = 10. Three of the six sources, including the two brightest, are in a single WFC3 pointing (∼4 arcmin2), suggestive of significant clustering, which is expected from bright galaxies at z ∼ 10. However, the two brightest galaxies are too extended to be likely at z ∼ 10, and one additional source is unresolved and possibly a brown dwarf. The remaining three candidates have mAB ∼ 26, and given the area and completeness of our search, our best estimate is a number density of sources that is marginally higher but consistent at 2 with searches in legacy fields. Our study highlights that z ∼ 10 searches can yield a small number of candidates, making tailored follow-ups of HST pure-parallel observations viable and effective.
Purpose
This study aims to evaluate the association of the maximum standardized uptake value (SUVmax) in positron-emission tomography targeting prostate-specific membrane antigen (PSMA-PET) prior to ...salvage radiotherapy (sRT) on biochemical recurrence free survival (BRFS) in a large multicenter cohort.
Methods
Patients who underwent
68
Ga-PSMA11-PET prior to sRT were enrolled in four high-volume centers in this retrospective multicenter study. Only patients with PET-positive local recurrence (LR) and/or nodal recurrence (NR) within the pelvis were included. Patients were treated with intensity-modulated-sRT to the prostatic fossa and elective lymphatics in case of nodal disease. Dose escalation was delivered to PET-positive LR and NR. Androgen deprivation therapy was administered at the discretion of the treating physician. LR and NR were manually delineated and SUVmax was extracted for LR and NR. Cox-regression was performed to analyze the impact of clinical parameters and the SUVmax-derived values on BRFS.
Results
Two hundred thirty-five patients with a median follow-up (FU) of 24 months were included in the final cohort. Two-year and 4-year BRFS for all patients were 68% and 56%. The presence of LR was associated with favorable BRFS (
p
= 0.016). Presence of NR was associated with unfavorable BRFS (
p
= 0.007). While there was a trend for SUVmax values ≥ median (
p
= 0.071), SUVmax values ≥ 75% quartile in LR were significantly associated with unfavorable BRFS (
p
= 0.022, HR: 2.1, 95%CI 1.1–4.6). SUVmax value in NR was not significantly associated with BRFS. SUVmax in LR stayed significant in multivariate analysis (
p
= 0.030). Sensitivity analysis with patients for who had a FU of > 12 months (
n
= 197) confirmed these results.
Conclusion
The non-invasive biomarker SUVmax can prognosticate outcome in patients undergoing sRT and recurrence confined to the prostatic fossa in PSMA-PET. Its addition might contribute to improve risk stratification of patients with recurrent PCa and to guide personalized treatment decisions in terms of treatment intensification or de-intensification.
This article is part of the Topical Collection on Oncology—Genitourinary.
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DOBA, EMUNI, FIS, FZAB, GEOZS, GIS, IJS, IMTLJ, IZUM, KILJ, KISLJ, MFDPS, NLZOH, NUK, OILJ, PILJ, PNG, SAZU, SBCE, SBJE, SBMB, SBNM, SIK, UILJ, UKNU, UL, UM, UPUK, VKSCE, VSZLJ, ZAGLJ
We present a study of the intersection between the populations of star forming galaxies selected as either Lyman break galaxies (LBGs) or Lyman-alpha emitters (LAEs) in the redshift range 2.9 − 6.7 ...and within the same volume of universe sampled by the Multi-Unit Spectroscopic Explorer (MUSE) behind the
Hubble
Frontier Fields lensing cluster A2744. We define three samples of star-forming galaxies: LBG galaxies with an LAE counterpart (92 galaxies), LBG galaxies without an LAE counterpart (408 galaxies), and LAE galaxies without an LBG counterpart (46 galaxies). All these galaxies are intrinsically faint because of the lensing nature of the sample (
M
1500
≥ −20.5). The fraction of LAEs among all selected star-forming galaxies increases with redshift up to
z
∼ 6 and decreases for higher redshifts, in agreement with previous findings. The evolution of LAE/LBG populations with UV magnitude and Ly
α
luminosity shows that the LAE selection is able to identify intrinsically UV faint galaxies with
M
1500
≥ −15 that are typically missed in the deepest lensing photometric surveys. The LBG population seems to fairly represent the total population of star-forming galaxies down to
M
1500
∼ −15. Galaxies with
M
1500
< −17 tend to have SFR
Ly
α
< SFR
uv
, whereas the opposite trend is observed within our sample for faint galaxies with
M
1500
> −17, including galaxies only detected by their Ly
α
emission, with a large scatter. These trends, previously observed in other samples of star-forming galaxies at high-
z
, are seen here for very faint
M
1500
∼ −15 galaxies; that is, much fainter than in previous studies. The present results show no clear evidence for an intrinsic difference between the properties of the two populations selected as LBG and/or LAE. The observed trends could be explained by a combination of several phenomena, like the existence of different star-formation regimes, the dust content, the relative distribution and morphology of dust and stars, or the stellar populations.
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