551 research outputs found
Advances in biotechnology: genomics and genome editing
Genomics, the study of genes, their functions and related techniques has become a crucial science for developing understanding of life processes and how they evolve. Since the advent of the human genome project, huge strides have been made in developing understanding of DNA and RNA sequence information and how it can be put to good use in the biotechnology sector. Newly derived sequencing and bioinformatics tools have added to the torrent of new insights gained, so that 'sequence once and query often' type DNA apps are now becoming reality. Genome editing, using tools such as CRISPR/Cas9 nuclease or Cpf1 nuclease, provide rapid methods for inserting, deleting or modifying DNA sequences in highly precise ways, in virtually any animal, plant or microbial system. Recent international discussions have considered human germline gene editing, amongst other aspects of this technology. Whether or not gene edited plants will be considered as genetically modified remains an important question. This will determine the regulatory processes adopted by different groups of nations and applicability to feeding the world's ever growing population. Questions surrounding the intellectual property rights associated with gene editing must also be resolved. Mitochondrial replacement therapy leading to '3-Parent Babies' has been successfully carried out in Mexico, by an international team, to correct mother to child mitochondrial disease transmission. The UK has become the first country to legally allow 'cautious use' of mitochondrial donation in treatment. Genomics and genome editing will continue to advance what can be achieved technically, whilst society determines whether or not what can be done should be applied
Analysis of the Combustion Process in a Hydrogen-Fueled CFR Engine
Green hydrogen, produced using renewable energy, is nowadays one of the most promising alternatives to fossil fuels for reducing pollutant emissions and in turn global warming. In particular, the use of hydrogen as fuel for internal combustion engines has been widely analyzed over the past few years. In this paper, the authors show the results of some experimental tests performed on a hydrogen-fueled CFR (Cooperative Fuel Research) engine, with particular reference to the combustion. Both the air/fuel (A/F) ratio and the engine compression ratio (CR) were varied in order to evaluate the influence of the two parameters on the combustion process. The combustion duration was divided in two parts: the flame front development (characterized by laminar flame speed) and the rapid combustion phase (characterized by turbulent flame speed). The results of the hydrogen-fueled engine have been compared with results obtained with gasoline in a reference operating condition. The increase in engine CR reduces the combustion duration whereas the opposite effect is observed with an increase in the A/F ratio. It is interesting to observe how the two parameters, CR and A/F ratio, have a different influence on the laminar and turbulent combustion phases. The influence of both A/F ratio and engine CR on heat transfer to the combustion chamber wall was also evaluated and compared with the gasoline operation. The heat transfer resulting from hydrogen combustion was found to be higher than the heat transfer resulting from gasoline combustion, and this is probably due to the different quenching distance of the two fuels
The extended structure of the dwarf irregular galaxy Sagittarius
We present a detailed study of the stellar and HI structure of the dwarf
irregular galaxy Sagittarius. We use new deep and wide field photometry to
trace the surface brightness profile of the galaxy out to ~5.0' (corresponding
to ~1600 pc) and down to mag/arcsec, thus showing that
the stellar body of the galaxy is much more extended than previously believed,
and it is similarly (or more) extended than the overall HI distribution. The
whole major-axis profile is consistent with a pure exponential, with a scale
radius of pc. The surface density maps reveal that the
distribution of old and intermediate-age stars is smooth and remarkably
flattened out to its edges, while the associated HI has a much rounder shape,
is off-centred and presents multiple density maxima and a significant hole. No
clear sign of systemic rotation is detectable in the complex HI velocity field.
No metallicity gradient is detected in the old and intermediate age population
of the galaxy, and we confirm that this population has a much more extended
distribution than young stars (age Gyr).Comment: 11 pages, 14 figures, accepted for publication on A&A. arXiv admin
note: text overlap with arXiv:1404.169
The extended structure of the dwarf irregular galaxies Sextans A and Sextans B. Signatures of tidal distortion in the outskirts of the Local Group
We present a detailed study of the stellar and HI structure of the dwarf
irregular galaxies SextansA and SextansB, members of the NGC3109 association.
We use newly obtained deep (r~26.5) and wide field g,r photometry to extend the
Surface Brightness (SB) profiles of the two galaxies down to mu_V~ 31.0
mag/arcsec^2. We find that both galaxies are significantly more extended than
what previously traced with surface photometry, out to ~4 kpc from their
centers along their major axis. Older stars are found to have more extended
distribution with respect to younger populations. We obtain the first estimate
of the mean metallicity for the old stars in SexB, from the color distribution
of the Red Giant Branch, =-1.6. The SB profiles show significant
changes of slope and cannot be fitted with a single Sersic model. Both galaxies
have HI discs as massive as their respective stellar components. In both cases
the HI discs display solid-body rotation with maximum amplitude of ~50 km/s
(albeit with significant uncertainty due to the poorly constrained
inclination), implying a dynamical mass ~10^{9}~M_sun, a mass-to-light ratio
M/L_V~25 and a dark-to-barionic mass ratio of ~10. The distribution of the
stellar components is more extended than the gaseous disc in both galaxies. We
find that the main, approximately round-shaped, stellar body of Sex~A is
surrounded by an elongated low-SB stellar halo that can be interpreted as a
tidal tail, similar to that found in another member of the same association
(Antlia). We discuss these, as well as other evidences of tidal disturbance, in
the framework of a past passage of the NGC3109 association close to the Milky
Way, that has been hypothesized by several authors and is also supported by the
recently discovered filamentary configuration of the association itself.Comment: Accepted for publication by A&A. PdfLateX, 16 pages, 11 figures, 2
appendice
A Panchromatic Study of the Globular Cluster NGC 1904. I: The Blue Straggler Population
By combining high-resolution (HST-WFPC2) and wide-field ground based (2.2m
ESO-WFI) and space (GALEX) observations, we have collected a multi-wavelength
photometric data base (ranging from the far UV to the near infrared) of the
galactic globular cluster NGC1904 (M79). The sample covers the entire cluster
extension, from the very central regions up to the tidal radius. In the present
paper such a data set is used to study the BSS population and its radial
distribution. A total number of 39 bright () BSS has been
detected, and they have been found to be highly segregated in the cluster core.
No significant upturn in the BSS frequency has been observed in the outskirts
of NGC 1904, in contrast to other clusters (M 3, 47 Tuc, NGC 6752, M 5) studied
with the same technique. Such evidences, coupled with the large radius of
avoidance estimated for NGC 1904 ( core radii), indicate that
the vast majority of the cluster heavy stars (binaries) has already sunk to the
core. Accordingly, extensive dynamical simulations suggest that BSS formed by
mass transfer activity in primordial binaries evolving in isolation in the
cluster outskirts represent only a negligible (0--10%) fraction of the overall
population.Comment: ApJ accepte
Deep infrared observations of the puzzling central X-ray source in RCW103
1E 161348-5055 (1E 1613) is a point-like, soft X-ray source originally
identified as a radio-quiet, isolated neutron star, shining at the center of
the 2000 yr old supernova remnant RCW103. 1E 1613 features a puzzling 6.67 hour
periodicity as well as a dramatic variability over a time scale of few years.
Such a temporal behavior, coupled to the young age and to the lack of an
obvious optical counterpart, makes 1E 1613 a unique source among all compact
objects associated to SNRs. It could either be the first low-mass X-ray binary
system discovered inside a SNR, or a peculiar isolated magnetar with an
extremely slow spin period. Analysis of archival IR observations, performed in
2001 with the VLT/ISAAC instrument, and in 2002 with the NICMOS camera onboard
HST unveils a very crowded field. A few sources are positionally consistent
with the refined X-ray error region that we derived from the analysis of 13
Chandra observations. To shed light on the nature of 1E 1613, we have performed
deep IR observations of the field with the NACO instrument at the ESO/VLT,
searching for variability. We find no compelling reasons to associate any of
the candidates to 1E 1613. On one side, within the frame of the binary system
model for the X-ray source, it is very unlikely that one of the candidates be a
low-mass companion star to 1E 1613. On the other side, if the X-ray source is
an isolated magnetar surrounded by a fallback disc, we cannot exclude that the
IR counterpart be hidden among the candidates. If none of the potential
counterparts is linked to the X-ray source, 1E 1613 would remain undetected in
the IR down to Ks>22.1. Such an upper limit is consistent only with an
extremely low-mass star (an M6-M8 dwarf) at the position of 1E 1613, and makes
rather problematic the interpretation of 1E 1613 as an accreting binary system.Comment: 26 pages, 5 figures. Accepted for publication in Ap
Technical-economic comparison of chemical precipitation and ion exchange processes for the removal of phosphorus from wastewater
Chemical precipitation with the addition of ferric chloride is commonly used to remove phosphorus from wastewater. However, since its application also involves several disadvantages, alternative solutions are required. The present paper shows the results of a full-scale experimental work aimed at evaluating the efficiency of the ion exchange process using a polymeric anion exchange resin impregnated with aluminum ions in the removal of phosphorus from wastewater. The study compared the results obtained through this process with chemical precipitation, considering both technical and economic issues. At the same dosage of 6 L/hour and influent concentration (about 6 mg/L), total removal efficiency of 95% and 78% (including also that occurring in the mechanical and biological processes) was achieved by means of the anion exchange process and chemical precipitation, respectively. However, in the latter case, this value was insufficient to ensure consistent compliance with the limit of 2 mg/L Ptot set on the effluent; to achieve this goal, the ferric chloride dosage had to be raised to 12 L/hour, thus increasing the related costs. Furthermore, the anion exchange process generated a lower sludge production. Therefore, the ion exchange process represents a valid alternative to chemical precipitation for P removal from wastewater
Lithium abundances in globular cluster giants: NGC 1904, NGC 2808, and NGC 362
The presence of multiple populations in globular clusters has been well
established thanks to high-resolution spectroscopy. It is widely accepted that
distinct populations are a consequence of different stellar generations:
intra-cluster pollution episodes are required to produce the peculiar chemistry
observed in almost all clusters. Unfortunately, the progenitors responsible
have left an ambiguous signature and their nature remains unresolved. To
constrain the candidate polluters, we have measured lithium and aluminium
abundances in more than 180 giants across three systems: NGC~1904, NGC~2808,
and NGC~362. The present investigation along with our previous analysis of M12
and M5 affords us the largest database of simultaneous determinations of Li and
Al abundances. Our results indicate that Li production has occurred in each of
the three clusters. In NGC~362 we detected an M12-like behaviour, with first
and second-generation stars sharing very similar Li abundances favouring a
progenitor that is able to produce Li, such as AGB stars. Multiple progenitor
types are possible in NGC~1904 and NGC~2808, as they possess both an
intermediate population comparable in lithium to the first generation stars and
also an extreme population, that is enriched in Al but depleted in Li. A simple
dilution model fails in reproducing this complex pattern. Finally, the internal
Li variation seems to suggest that the production efficiency of this element is
a function of the cluster's mass and metallicity - low-mass or relatively
metal-rich clusters are more adept at producing Li.Comment: Accepted for publication in MNRAS. 10 pages, 8 figure
A super lithium-rich red-clump star in the open cluster Trumpler 5
Context. The existence of lithium-rich low-mass red giant stars still
represents a challenge for stellar evolution models. Stellar clusters are
privileged environments for this kind of investigation. Aims. To investigate
the chemical abundance pattern of the old open cluster Trumpler\,5, we observed
a sample of four red-clump stars with high-resolution optical spectrographs.
One of them (#3416) reveals extremely strong lithium lines in its spectrum.
Methods. One-dimensional, local thermodynamic equilibrium analysis was
performed on the spectra of the observed stars. A 3D-NLTE analysis was
performed to derive the lithium abundance of star #3416. Results. Star #3416 is
super Li-rich with A(Li)=3.75\,dex. The lack of Li enrichment
(Li/Li2%), the low carbon isotopic ratio
(C/C=143), and the lack of evidence for radial velocity
variation or enhanced rotational velocity (\kms) all suggest
that lithium production has occurred in this star through the Cameron & Fowler
mechanism. Conclusions. We identified a super Li-rich core helium-burning,
red-clump star in an open cluster. Internal production is the most likely cause
of the observed enrichment. Given the expected short duration of a star's
Li-rich phase, enrichment is likely to have occurred at the red clump or in the
immediately preceding phases, namely during the He-flash at the tip of the red
giant branch (RGB) or while ascending the brightest portion of the RGB.Comment: 7 pages, 2 figures. Accepted for publication in A&A Letter
Double Blue Straggler sequences in GCs: the case of NGC 362
We used high-quality images acquired with the WFC3 on board the HST to probe
the blue straggler star (BSS) population of the Galactic globular cluster NGC
362. We have found two distinct sequences of BSS: this is the second case,
after M 30, where such a feature has been observed. Indeed the BSS location,
their extension in magnitude and color and their radial distribution within the
cluster nicely resemble those observed in M 30, thus suggesting that the same
interpretative scenario can be applied: the red BSS sub-population is generated
by mass transfer binaries, the blue one by collisions. The discovery of four
new W UMa stars, three of which lying along the red-BSS sequence, further
supports this scenario. We also found that the inner portion of the density
profile deviates from a King model and is well reproduced by either a mild
power-law (\alpha -0.2) or a double King profile. This feature supports the
hypothesis that the cluster is currently undergoing the core collapse phase.
Moreover, the BSS radial distribution shows a central peak and monotonically
decreases outward without any evidence of an external rising branch. This
evidence is a further indication of the advanced dynamical age of NGC 362: in
fact, together with M 30, NGC 362 belongs to the family of dynamically old
clusters (Family III) in the "dynamical clock" classification proposed by
Ferraro et al. (2012). The observational evidence presented here strengthens
the possible connection between the existence of a double BSS sequence and a
quite advanced dynamical status of the parent cluster.Comment: Accepted for publication by ApJ; 39 pages, 16 figures, 1 tabl
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