In this article, we shall study the mechanism of the Shroud body image formation with the help of both natural sciences and religion. The various possibilities can be divided into three groups of ...hypothesis: the first one is that of the fake, the second is the miracle and the third one of the natural event. The first hypothesis is discarded by the interdisciplinary work of the STURP (The Shroud of Turin Research Project) team. Their results do not support the hypothesis that the blood stains and the body image are due to a forger. In our opinion, even if the Miracle by God is possible, the proposed hypotheses of the supernatural event are theologically unacceptable. So, the natural one remains well supported by the “Ockham’s razor”. Obviously, this last model must be verified by experimental evidence. However, this result is not contrary to the hypothesis that the body image is the one of the Nazarene.
We examine the effects of pre-processing across the Coma Supercluster, including 3505 galaxies over ∼500 deg2, by quantifying the degree to which star-forming (SF) activity is quenched as a function ...of environment. We characterize environment using the complementary techniques of Voronoi Tessellation, to measure the density field, and the Minimal Spanning Tree, to define continuous structures, and so we measure SF activity as a function of local density and the type of environment (cluster, group, filament, and void), and quantify the degree to which environment contributes to quenching of SF activity. Our sample covers over two orders of magnitude in stellar mass (108.5-1011 M), and consequently, we trace the effects of environment on SF activity for dwarf and massive galaxies, distinguishing so-called mass quenching from environment quenching. Environmentally driven quenching of SF activity, measured relative to the void galaxies, occurs to progressively greater degrees in filaments, groups, and clusters, and this trend holds for dwarf and massive galaxies alike. A similar trend is found using g − r colours, but with a more significant disparity between galaxy mass bins driven by increased internal dust extinction in massive galaxies. The SFR distributions of massive SF galaxies have no significant environmental dependence, but the distributions for dwarf SF galaxies are found to be statistically distinct in most environments. Pre-processing plays a significant role at low redshift, as environmentally driven galaxy evolution affects nearly half of the galaxies in the group environment, and a significant fraction of the galaxies in the more diffuse filaments. Our study underscores the need for sensitivity to dwarf galaxies to separate mass-driven from environmentally driven effects, and the use of unbiased tracers of SF activity.
ABSTRACT One of the most challenging aspects of studying galaxies in the universe is the infrequent confirmation of their redshifts through spectroscopy, a phenomenon thought to occur from the ...increasing opacity of the intergalactic medium to Ly photons at . The resulting redshift uncertainties inhibit the efficient search for C ii in galaxies with sub-millimeter instruments such as ALMA, given their limited scan speed for faint lines. One means by which to improve the precision of the inferred redshifts is to exploit the potential impact of strong nebular emission lines on the colors of z ∼ 4 - 8 galaxies as observed by Spitzer/IRAC. At , galaxies exhibit IRAC colors as blue as , likely due to the contribution of O iii+Hβ to the 3.6 m flux combined with the absence of line contamination in the 4.5 m band. In this paper we explore the use of extremely blue colors to identify galaxies in the narrow redshift window 6.6 - 6.9. When combined with an I-dropout criterion, we demonstrate that we can plausibly select a relatively clean sample of galaxies. Through a systematic application of this selection technique to our catalogs from all five CANDELS fields, we identify 20 probable 6.6 - 6.9 galaxies. We estimate that our criteria select the ∼50% strongest line emitters at and from the IRAC colors we estimate a typical O iii rest-frame equivalent width of 1085 for this sample. The small redshift uncertainties on our sample make it particularly well suited for follow-up studies with facilities such as ALMA.
The total infrared (IR) luminosity is very useful for estimating the star formation rate (SFR) of galaxies, but converting the IR luminosity into an SFR relies on assumptions that do not hold for all ...galaxies. We test the effectiveness of the IR luminosity as an SFR indicator by applying it to synthetic spectral energy distributions generated from three-dimensional hydrodynamical simulations of isolated disc galaxies and galaxy mergers. In general, the SFR inferred from the IR luminosity agrees well with the true instantaneous SFR of the simulated galaxies. However, for the major mergers in which a strong starburst is induced, the SFR inferred from the IR luminosity can overestimate the instantaneous SFR during the post-starburst phase by greater than two orders of magnitude. Even though the instantaneous SFR decreases rapidly after the starburst, the stars that were formed in the starburst can remain dust-obscured and thus produce significant IR luminosity. Consequently, use of the IR luminosity as an SFR indicator may cause one to conclude that post-starburst galaxies are still star forming, whereas in reality, star formation was recently quenched.
Abstract
We constrain the emission mechanisms responsible for the prodigious electromagnetic output generated by active galactic nuclei (AGNs) and their host galaxies with a novel state-of-the-art ...AGN radio-to-X-ray spectral energy distribution model fitting code (ARXSED). ARXSED combines multiple components to fit the spectral energy distributions (SEDs) of AGNs and their host galaxies. Emission components include radio structures such as lobes and jets, infrared emission from the AGN torus, visible-to-X-ray emission from the accretion disk, and radio-to-ultraviolet emission from the host galaxy. Applying ARXSED to the radio SEDs of 20 3CRR quasars at 1 <
z
< 2 verifies the need for more than a simple power law when compact radio structures are present. The nonthermal emission contributes 91%–57% of the observed-frame 1.25 mm to 850
μ
m flux, and this component must be accounted for when using these wavelengths to estimate star formation properties. We predict the presence of strong radio-linked X-ray emission in more than half the sample sources. ARXSED estimates median (and the associated first and third quartile ranges) BH mass of
2.9
1.7
6.0
×
10
9
M
☉
, logarithm of Eddington ratio of
−
1.0
−
1.2
−
0.6
, and spin of
0.98
0.94
0.99
for our sample. The inferred AGN torus and accretion disk parameters agree with those estimated from spectroscopic analyses of similar samples in the literature. We present the median intrinsic SED of the luminous radio-loud quasars at 1 <
z
≲ 2; this SED represents a significant improvement in the way each component is modeled.
Abstract
The James Webb Space Telescope Time-Domain Field (JWST-TDF) is an ∼14′ diameter field near the North Ecliptic Pole that will be targeted by one of the JWST Guaranteed Time Observations ...programs. Here, we describe our James Clerk Maxwell Telescope SCUBA-2 850
μ
m imaging of the JWST-TDF and present the submillimeter source catalog and properties. We also present a catalog of radio sources from Karl J. Jansky Very Large Array 3 GHz observations of the field. These observations were obtained to aid JWST's study of dust-obscured galaxies that contribute significantly to cosmic star formation at high redshifts. Our deep 850
μ
m map covers the JWST-TDF at a noise level of
σ
850
µ
m
= 1.0 mJy beam
−1
, detecting 83/31 sources in the main/supplementary signal-to-noise ratio (S/N > 4 / S/N = 3.5–4) sample, respectively. The 3 GHz observations cover a 24′ diameter field with a 1
σ
noise of 1
μ
Jy beam
−1
at a 0.″7 FWHM. We identified eighty-five 3 GHz counterparts to sixty-six 850
μ
m sources and then matched these with multiwavelength data from the optical to the mid-infrared wave bands. We performed spectral energy distribution fitting for 61 submillimeter galaxies (SMGs) matched with optical/near-infrared data, and found that SMGs at S/N > 4 have a median value of
z
phot
= 2.22 ± 0.12, star formation rates of 300 ± 40
M
⊙
yr
−1
(Chabrier initial mass function), and typical cold dust masses of 5.9 ± 0.7 × 10
8
M
⊙
, in line with bright SMGs from other surveys. The large cold dust masses indicate correspondingly large cool gas masses, which we suggest are a key factor necessary to drive the high star formation rates seen in this population.
Recent evidence suggests that oxidative stress and endothelial dysfunction play critical roles in the pathophysiology of COVID-19 and Long-COVID. We hypothesized that a supplementation combining ...L-Arginine (to improve endothelial function) and Vitamin C (to reduce oxidation) could have favorable effects on Long-COVID symptoms.
We designed a survey (LINCOLN: L-Arginine and Vitamin C improves Long-COVID), assessing several symptoms that have been associated with Long-COVID to be administered nationwide to COVID-19 survivors; the survey also included effort perception, measured using the Borg scale. Patients receiving the survey were divided in two groups, with a 2:1 ratio: the first group included patients that received L-Arginine + Vitamin C, whereas the second group received a multivitamin combination (alternative treatment).
1390 patients successfully completed the survey. Following a 30-day treatment in both groups, the survey revealed that patients in the L-Arginine + Vitamin C treatment arm had significantly lower scores compared to patients who had received the multivitamin combination. There were no other significant differences between the two groups. When examining effort perception, we observed a significantly lower value (p < 0.0001) in patients receiving L-Arginine + Vitamin C compared to the alternative-treatment arm.
Our survey indicates that the supplementation with L-Arginine + Vitamin C has beneficial effects in Long-COVID, in terms of attenuating its typical symptoms and improving effort perception.
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•We hypothesized that a supplementation combining L-Arginine (to improve endothelial function) and Vitamin C (to reduce oxidation) could have beneficial effects in Long-COVID.•We designed a survey administered nationwide to COVID-19 survivors to assess several symptoms that have been associated with Long-COVID.•1390 patients – divided in two groups L-Arginine + Vitamin C vs multivitaminic combinations (alternative treatment) – completed the survey.•After 1-month treatment, patients in the L-Arginine + Vitamin C group had significantly lower scores compared to the alternative treatment group.
ABSTRACT Recent observations have shown that the characteristic luminosity of the rest-frame ultraviolet (UV) luminosity function does not significantly evolve at 4 < z < 7 and is approximately We ...investigate this apparent non-evolution by examining a sample of 173 bright, MUV < −21 galaxies at z = 4-7, analyzing their stellar populations and host halo masses. Including deep Spitzer/IRAC imaging to constrain the rest-frame optical light, we find that galaxies at z = 4-7 have similar stellar masses of log(M/M ) = 9.6-9.9 and are thus relatively massive for these high redshifts. However, bright galaxies at z = 4-7 are less massive and have younger inferred ages than similarly bright galaxies at z = 2-3, even though the two populations have similar star formation rates and levels of dust attenuation for a fixed dust-attenuation curve. Matching the abundances of these bright z = 4-7 galaxies to halo mass functions from the Bolshoi ΛCDM simulation implies that the typical halo masses in galaxies decrease from log(Mh/M ) = 11.9 at z = 4 to log(Mh/M ) = 11.4 at z = 7. Thus, although we are studying galaxies at a similar stellar mass across multiple redshifts, these galaxies live in lower mass halos at higher redshift. The stellar baryon fraction in galaxies in units of the cosmic mean b/ m rises from 5.1% at z = 4 to 11.7% at z = 7; this evolution is significant at the ∼3 level. This rise does not agree with simple expectations of how galaxies grow, and implies that some effect, perhaps a diminishing efficiency of feedback, is allowing a higher fraction of available baryons to be converted into stars at high redshifts.
We report on the identification of the old stellar population galaxy candidates at z ≳ 5. We developed a new infrared color selection scheme to isolate galaxies with the strong Balmer breaks at z ≳ ...5, and applied it to the ultra-deep and wide infrared survey data from the Spitzer Extended Deep Survey (SEDS) and the UKIRT Infrared Deep Sky Survey. The eight objects satisfying K − 3.6 > 1.3 and K − 3.6 > 2.4(3.6 − 4.5) + 0.6 are selected in the 0.34 deg2 SEDS Ultra Deep Survey field. Rich multi-wavelength imaging data from optical to far-infrared are also used to reject blending sources and strong nebular line emitters, and we finally obtained the three most likely evolved galaxies at z ≳ 5. Their stacked spectral energy distribution is fitted well with the old stellar population template with M* = (7.5 ± 1.5) × 1010 M⊙, star formation rate = 0.9 ± 0.2 M⊙ yr−1, dust AV < 1, and age =0.7 ± 0.4 Gyr at z = 5.7 ± 0.6, where the dusty star-forming galaxies at z ∼ 2.8 are disfavored because of the faintness in the 24 μm. The stellar mass density of these evolved galaxy candidates, (6 ± 4) × 104 M⊙ Mpc−3, is much lower than that of star-forming galaxies, but the non-zero fraction suggests that initial star-formation and quenching have been completed by z ∼ 6.
Abstract
We have used the Submillimeter Array (SMA) at 860 $\mu$m to observe the brightest sources in the Submillimeter Common User Bolometer Array-2 (SCUBA-2) Cosmology Legacy Survey (S2CLS). The ...goal of this survey is to exploit the large field of the S2CLS along with the resolution and sensitivity of the SMA to construct a large sample of these rare sources and to study their statistical properties. We have targeted 70 of the brightest single-dish SCUBA-2 850 $\mu$m sources down to S850 ≈ 8 mJy, achieving an average synthesized beam of 2.4 arcsec and an average rms of σ860 = 1.5 mJy beam−1 in our primary beam-corrected maps. We searched our SMA maps for 4σ peaks, corresponding to S860 ≳ 6 mJy sources, and detected 62, galaxies, including three pairs. We include in our study 35 archival observations, bringing our sample size to 105 bright single-dish submillimetre sources with interferometric follow-up. We compute the cumulative and differential number counts, finding them to overlap with previous single-dish survey number counts within the uncertainties, although our cumulative number count is systematically lower than the parent S2CLS cumulative number count by 14 ± 6 per cent between 11 and 15 mJy. We estimate the probability that a ≳10 mJy single-dish submillimetre source resolves into two or more galaxies with similar flux densities to be less than 15 per cent. Assuming the remaining 85 per cent of the targets are ultraluminous starburst galaxies between z = 2 and 3, we find a likely volume density of ≳400 M⊙ yr−1 sources to be ${\sim }\,3^{+0.7}_{-0.6}\,{\times }\,10^{-7}$ Mpc−3. We show that the descendants of these galaxies could be ≳4 × 1011 M⊙ local quiescent galaxies, and that about 10 per cent of their total stellar mass would have formed during these short bursts of star formation.
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