124 research outputs found
Optical coherence tomography- a non-invasive technique applied to conservation of paintings
It is current practice to take tiny samples from a painting to mount and examine in cross-section under a microscope. However, since conservation practice and ethics limit sampling to a minimum and to areas along cracks and edges of paintings, which are often unrepresentative of the whole painting, results from such analyses cannot be taken as representative of a painting as a whole. Recently in a preliminary study, we have demonstrated that near-infrared Optical Coherence Tomography (OCT) can be used directly on paintings to examine the cross-section of paint and varnish layers without contact and the need to take samples. OCT is an optical interferometric technique developed for in vivo imaging of the eye and biological tissues; it is essentially a scanning Michelsonâs interferometer with a âbroadbandâ source that has the spatial coherence of a laser. The low temporal coherence and high spatial concentration of the source are the keys to high depth resolution and high sensitivity 3D imaging. The technique is non-invasive and noncontact with a typical working distance of 2 cm. This non-invasive technique enables cross-sections to be examined anywhere on a painting. In this paper, we will report new results on applying near-infrared en-face OCT to paintings conservation and extend the application to the examination of underdrawings, drying processes, and quantitative measurements of optical properties of paint and varnish layers
New driver alterations in non-small cell lung cancer. A narrative review
Objective: This review aims to provide an up-to-date snapshot on the state of development of novel biomarker-driven treatments in non-small cell lung cancer (NSCLC).
Background: The introduction of immune checkpoint inhibitors and target therapies has revolutionized the natural history of many NSCLCs, allowing for lasting and profound responses. In particular, mutations in the epidermal growth factor receptor (EGFR), rearrangements of the anaplastic lymphoma kinase (ALK), or oncogene c-Ros 1 (ROS1) have marked a paradigm shift in the treatment of NSCLC. Furthermore, new inhibitors for B-Raf proto-oncogene (BRAF), rearranged during transfection (RET), mesenchymal-to-epithelial transition factor (MET), or neurotrophic tyrosine kinase (NTRK) 1â3 have revealed fascinating data, obtaining accelerated approvals from the Food and Drug Administration (FDA) and European Medicines Agency (EMA). Today, the extensive use of next-generation sequencing (NGS) techniques has shown a broad molecular heterogeneity of NSCLC. Many of the mutations identified are considered potential therapeutic targets, and numerous studies are currently evaluating the efficacy of selective inhibitors.
Methods: We carried out an extensive review of the literature on PubMed, Web of Science, and Scopus databases and the congress abstracts presented at the American Society of Clinical Oncology (ASCO), European Society for Medical Oncology (ESMO), and World Conference on Lung Cancer (WCLC) in the last 5 years. Our analysis considered works regarding new inhibitors for alterations of Kirsten rat sarcoma viral oncogene homolog (KRAS), PIK3CA, neuregulin-1 (NRG-1), human epidermal growth factor receptor 2 (HER2), fibroblast growth factor receptor (FGFR), genes that have recently become no longer undruggable.
Conclusions: Precision oncology is revolutionizing the natural history of NSCLC. Several alterations have been identified as possible treatment targets, and numerous inhibitors show promising results in ongoing clinical trials
Bimodal Color Distribution in Hierarchical Galaxy Formation
We show how the observed bimodality in the color distribution of galaxies can
be explained in the framework of the hierarchical clustering picture in terms
of the interplay between the properties of the merging histories and the
feedback/star-formation processes in the progenitors of local galaxies. Using a
semi-analytic model of hierarchical galaxy formation, we compute the color
distributions of galaxies with different luminosities and compare them with the
observations. Our fiducial model matches the fundamental properties of the
observed distributions, namely: 1) the distribution of objects brighter than
M_r = -18 is clearly bimodal, with a fraction of red objects increasing with
luminosity; 2) for objects brighter than M_r = -21 the color distribution is
dominated by red objects with color u-r = 2.2-2.4; 3) the spread on the
distribution of the red population is smaller than that of the blue population;
4) the fraction of red galaxies is larger in denser environments, even for
low-luminosity objects; 5) the bimodality in the distribution persists up to z
= 1.5. We discuss the role of the different physical processes included in the
model in producing the above results.Comment: 11 pages, accepted for publication in the Astrophysical Journa
The evolving slope of the stellar mass function at 0.6 <= z < 4.5 from deep WFC3 data
We used Early Release Science (ERS) observations taken with the Wide Field
Camera 3 (WFC3) in the GOODS-S field to study the galaxy stellar mass function
(GSMF) at 0.6<=z<4.5. Deep WFC3 near-IR data (for Y as faint as 27.3, J and H
as faint as 27.4 AB mag at 5 sigma), as well as deep Ks (as faint as 25.5 at 5
sigma) Hawk-I band data, provide an exquisite data set with which determine in
an unprecedented way the low-mass end of the GSMF, allowing an accurate probe
of masses as low as M~7.6 10^9 Msun at z~3. Although the area used is
relatively small (~33 arcmin^2), we found generally good agreement with
previous studies on the entire mass range. Our results show that the slope of
the faint-end increases with redshift, from alpha=-1.44+/-0.03 at z~0.8 to
alpha=-1.86+/-0.16 at z~3, although indications exist that it does not steepen
further between z~3 and z~4. This result is insensitive to any uncertainty in
the M* parameter. The steepness of the GSMF faint-end solves the well-known
disagreement between the stellar mass density (SMD) and the integrated star
formation history at z>2. However, we confirm the that there appears to be an
excess of integrated star formation with respect to the SMD at z<2, by a factor
of ~2-3. Our comparison of the observations with theoretical predictions shows
that the models forecast a greater abundance of low mass galaxies, at least up
to z~3, as well as a dearth of massive galaxies at z~4 with respect to the
data, and that the predicted SMD is generally overestimated at z<~2.Comment: Accepted for publication in Astronomy & Astrophysics. Minor language
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Evidence for a fast evolution of the UV luminosity function beyond redshift 6 from a deep HAWK-I survey of the GOODS-S field
We perform a deep search for galaxies in the redshift range 6.5<z<7.5, to
measure the evolution of the number density of luminous galaxies in this
redshift range and derive useful constraints on the evolution of their
Luminosity Function. We present here the first results of an ESO Large Program,
that exploits the unique combination of area and sensitivity provided in the
near-IR by the camera Hawk-I at the VLT. We have obtained two Hawk-I pointings
on the GOODS South field for a total of 32 observing hours, covering ~90
arcmin2. The images reach Y=26.7 mags for the two fields. We have used public
ACS images in the z band to select z-dropout galaxies with the colour criteria
Z-Y>1, Y-J<1.5 and Y-K<2. The other public data in the UBVRIJHK bands are used
to reject possible low redshift interlopers. The output has been compared with
extensive Monte Carlo simulations to quantify the observational effects of our
selection criteria as well as the effects of photometric errors. We detect 7
high quality candidates in the magnitude range Y=25.5-26.7. This interval
samples the critical range for M* at z>6 (M_1500 ~- 19.5 to -21.5). After
accounting for the expected incompleteness, we rule out at a 99% confidence
level a Luminosity Function constant from z=6 to z=7, even including the
effects of cosmic variance. For galaxies brighter than M_1500=-19.0 we derive a
luminosity density rho_UV=1.5^{+2.0}_{-0.9} 10^25 erg/s/Hz/Mpc3, implying a
decrease by a factor 3.5 from z=6 to z~6.8. On the basis of our findings, we
make predictions for the surface densities expected in future surveys surveys,
based on ULTRA-VISTA, HST-WFC3 or JWST-NIRCam, evaluating the best
observational strategy to maximise their impact.Comment: Accepted for publication in Astronomy & Astrophysic
The Morphology of Passively Evolving Galaxies at Z approximately 2 from HST/WFC3 Deep Imaging in the Hubble Ultradeep Field
We present near-IR images of six passive galaxies (SSFR< 10(exp -2)/ Gyr) at redshift 1.3 < z < 2.4 with stellar mass M approximately 10(exp 11) solar M, selected from the Great Observatories Origins Deep Survey (GOODS), obtained with the Hubble Space Telescope (HST) and the WFC3/IR camera. These images provide the deepest and highest angular resolution view of the optical rest-frame morphology of such systems to date. We find that the light profile of these galaxies is generally regular and well described by a Sersic model with index typical of today's spheroids. We confirm the existence of compact and massive early-type galaxies at z approximately 2: four out of six galaxies have r(sub e) approximately 1 kpc or less. The images reach limiting surface brightness mu approximates 26.5 mag/square arcsec in the F160W bandpass; yet there is no evidence of a faint halo in the galaxies of our sample, even in their stacked image. We also find very weak "morphological k-correction" in the galaxies between the rest-frame UV (from the ACS z-band), and the rest-frame optical (WFC3 H-band): the visual classification, Sersic indices and physical sizes of these galaxies are independent or only mildly dependent on the wavelength, within the errors. The presence of an active nucleus is suspected in two out of six galaxies (33%), opening the intriguing possibility that a large, presently unaccounted population of AGN is hosted in these galaxies, possibly responsible for the cessation of star formation
The K20 survey. VI. The Distribution of the Stellar Masses in Galaxies up to z~2
We present a detailed analysis of the stellar mass content of galaxies up to
z=2.5 in the K20 galaxy sample, that has a 92% spectroscopic completeness and a
complete multicolor coverage. We find that the M/L ratio decreases
with redshift: in particular, the average M/L ratio of early type galaxies
decreases with , with a scatter that is indicative of a range of
star--formation time-scales and redshift of formation. More important, the
typical M/L of massive early type galaxies is larger than that of less massive
ones, suggesting that their stellar population formed at higher z. The final
K20 galaxy sample spans a range of stellar masses from M*=10^9Msun to
M*=10^12Msun, with massive galaxies ($M*>10^11Msun) detected up to z~2. We
compute the Galaxy Stellar Mass Function at various z, of which we observe only
a mild evolution (i.e. by 20-30%) up to z~1. At z>1, the evolution of the GSMF
appears to be much faster: at z~2, about 35% of the present day stellar mass in
objects with M*~10^11Msun appear to have assembled. We also detect a change in
the physical nature of the most massive galaxies, since at z>1 a population of
massive star--forming galaxies progressively appears. We finally analyze our
results in the framework of Lambda-CDM hierarchical models. First, we show that
the large number of massive galaxies detected at high z does not violate any
fundamental Lambda-CDM constraint based on the number of massive DM halos.
Then, we compare our results with the predictions of renditions of both
semianalytic and hydro-dynamical models, that range from severe underestimates
to slight overestimates of the observed mass density at z<~2. We discuss how
the differences among these models are due to the different implementation of
the main physical processes. (Abridged)Comment: Accepted for publication on Astronomy & Astrophysic
Far-Ultraviolet and Far-Infrared Bivariate Luminosity Function of Galaxies: Complex Relation between Stellar and Dust Emission
Far-ultraviolet (FUV) and far-infrared (FIR) luminosity functions (LFs) of
galaxies show a strong evolution from to , but the FIR LF
evolves much stronger than the FUV one. The FUV is dominantly radiated from
newly formed short-lived OB stars, while the FIR is emitted by dust grains
heated by the FUV radiation field. It is known that dust is always associated
with star formation activity. Thus, both FUV and FIR are tightly related to the
star formation in galaxies, but in a very complicated manner. In order to
disentangle the relation between FUV and FIR emissions, we estimate the UV-IR
bivariate LF (BLF) of galaxies with {\sl GALEX} and {\sl AKARI} All-Sky Survey
datasets. Recently we invented a new mathematical method to construct the BLF
with given marginals and prescribed correlation coefficient. This method makes
use of a tool from mathematical statistics, so called "copula". The copula
enables us to construct a bivariate distribution function from given marginal
distributions with prescribed correlation and/or dependence structure. With
this new formulation and FUV and FIR univariate LFs, we analyze various FUV and
FIR data with {\sl GALEX}, {\sl Spitzer}, and {\sl AKARI} to estimate the UV-IR
BLF. The obtained BLFs naturally explain the nonlinear complicated relation
between FUV and FIR emission from star-forming galaxies. Though the faint-end
of the BLF was not well constrained for high- samples, the estimated linear
correlation coefficient was found to be very high, and is remarkably
stable with redshifts (from 0.95 at to 0.85 at ). This implies
the evolution of the UV-IR BLF is mainly due to the different evolution of the
univariate LFs, and may not be controlled by the dependence structure.Comment: 10 pages, 7 figures, Earth, Planets and Space, in pres
The PEP survey: clustering of infrared-selected galaxies and structure formation at z~2 in the GOODS South
ABRIDGED-This paper presents the first direct estimate of the 3D clustering
properties of far-infrared sources up to z~3. This has been possible thanks to
the Pacs Evolutionary Probe (PEP) survey of the GOODS South field performed
with the PACS instrument onboard the Herschel Satellite. An analysis of the
two-point correlation function over the whole redshift range spanned by the
data reports for the correlation length, r_0~6.3 Mpc and r_0~6.7 Mpc,
respectively at 100um and 160um, corresponding to dark matter halo masses
M>~10^{12.4} M_sun. Objects at z~2 instead seem to be more strongly clustered,
with r_0~19 Mpc and r_0~17 Mpc in the two considered PACS channels. This
dramatic increase of the correlation length between z~1 and z~2 is connected
with the presence of a wide, M>~10^{14} M_sun, filamentary structure which
includes more than 50% of the sources detected at z~2. An investigation of the
properties of such sources indicates the possibility for boosted star-forming
activity in those which reside within the overdense environment with respect of
more isolated galaxies found in the same redshift range. Lastly, we also
present our results on the evolution of the relationship between luminous and
dark matter in star-forming galaxies between z~1 and z~2. We find that the
increase of (average) stellar mass in galaxies between z~1 and z~2 is
about a factor 10 lower than that of the dark matter haloes hosting such
objects ([z~1]/[z~2] ~ 0.4 vs M_{halo}[z~1]/M_{halo}[z~2] ~ 0.04). Our
findings agree with the evolutionary picture of downsizing whereby massive
galaxies at z~2 were more actively forming stars than their z~1 counterparts,
while at the same time contained a lower fraction of their mass in the form of
luminous matter.Comment: 14 pages, 8 figures, MNRAS accepte
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