85 research outputs found
The mass and environmental dependence on the secular processes of AGN in terms of morphology, colour, and specific star-formation rate
Galaxy mass and environment play a major role in the evolution of galaxies.
In the transition from star-forming to quenched galaxies, Active galactic
nuclei (AGN) have also a principal action. However, the connections between
these three actors are still uncertain. In this work we investigate the effects
of stellar mass and the large-scale environment (LSS), on the fraction of
optical nuclear activity in a population of isolated galaxies, where AGN would
not be triggered by recent galaxy interactions or mergers. As a continuation of
a previous work, we focus on isolated galaxies to study the effect of stellar
mass and the LSS in terms of morphology (early- and late-type), colour (red and
blue), and specific star formation rate (quenched and star-forming). To explore
where AGN activity is affected by the LSS we fix the stellar mass into low- and
high-mass galaxies. We use the tidal strength parameter to quantify their
effects. We found that AGN is strongly affected by stellar mass in 'active'
galaxies (namely late-type, blue, and star-forming), however it has no
influence for 'quiescent' galaxies (namely early-type, red, and quenched), at
least for masses down to . In relation to the LSS, we
found an increment on the fraction of SFN with denser LSS in low-mass star
forming and red isolated galaxies. Regarding AGN, we find a clear increment of
the fraction of AGN with denser environment in quenched and red isolated
galaxies, independently of the stellar mass. AGN activity would be 'mass
triggered' in 'active' isolated galaxies. This means that AGN is independent of
the intrinsic property of the galaxies, but on its stellar mass. On the other
hand, AGN would be 'environment triggered' in 'quiescent' isolated galaxies,
where the fraction of AGN in terms of sSFR and colour increases from void
regions to denser LSS, independently of its stellar mass.Comment: 14 pages, 9 figures (11 pages and 6 figures without appendix),
accepted for publication in Astronomy & Astrophysic
Isolated Galaxies versus Interacting Pairs with MaNGA
We present preliminary results of the spectral analysis on the radial
distributions of the star formation history in both, a galaxy merger and a
spiral isolated galaxy observed with MaNGA. We find that the central part of
the isolated galaxy is composed by older stellar population (2 Gyr) than
in the outskirts (7 Gyr). Also, the time-scale is gradually larger from 1
Gyr in the inner part to 3 Gyr in the outer regions of the galaxy. In the case
of the merger, the stellar population in the central region is older than in
the tails, presenting a longer time-scale in comparison to central part in the
isolated galaxy. Our results are in agreement with a scenario where spiral
galaxies are built from inside-out. In the case of the merger, we find evidence
that interactions enhance star formation in the central part of the galaxy.Comment: 7 pages, 2 figures. Proceedings of the EWASS-2015 special session
Sp3, accepted for publication in Special Issue "3D View on Interacting and
Post-Interacting Galaxies from Clusters to Voids" of open access journal
"Galaxies
The less significant role of large-scale environment than optical AGN in nearby, isolated elliptical galaxies
The formation and evolution of elliptical galaxies in low-density
environments are less understood than classical elliptical galaxies in
high-density environments. Isolated galaxies are defined as galaxies without
massive neighbors within scales of galaxy groups. The effect of the environment
at several Mpc scales on their properties has been barely explored. Here we
study the role of large-scale environment in some physical properties of 573
isolated elliptical galaxies out to z=0.08. We use three environmental
estimators of the large-scale structure within a projected radius of 5 Mpc
around isolated galaxies: the tidal strength parameter, the projected density
eta_k, and the distance to the fifth nearest neighbor galaxy. We find 80% of
galaxies at lower densities correspond to 'red and dead' elliptical galaxies.
Blue and red galaxies do not tend to be located in different environments
according to eta_k. Almost all the isolated ellipticals in the densest
large-scale environments are red or quenched, where a third of them are
low-mass galaxies. The percentage of isolated elliptical galaxies located in
the AGN region of the BPT diagram is 64%. We have identified 33 blue,
star-forming isolated ellipticals using both color and sSFR. Half of them are
star-forming nuclei in the BPT diagram, which is 5% of the galaxies in this
diagram. The large-scale environment is not playing the primary role to
determine the color or sSFR of isolated elliptical galaxies. The large-scale
environment seems to be negligible from a stellar mass scale around 10^10.6
Msun, probably because of the dominant presence of AGN at higher masses. For
lower masses, the processes of cooling and infall of gas from large scales are
very inefficient in ellipticals. AGN might also be an essential ingredient to
keep most of the low-mass isolated elliptical galaxies quenched.Comment: 15 pages, 6 figures (10 pages and 4 figures without appendices).
Accepted for publication in A&
Effects of the environment on galaxies in the Catalogue of Isolated Galaxies: physical satellites and large scale structure
We aim to identify and quantify the effects of the satellite distribution
around a sample of galaxies in the Catalogue of Isolated Galaxies (CIG), as
well as the effects of the Large Scale Structure (LSS) using the SDSS-DR9. To
recover the physically bound galaxies we focus on the satellites which are
within the escape speed of each CIG galaxy. We also propose a more conservative
method using the stacked Gaussian distribution of the velocity difference of
the neighbours. The tidal strengths affecting the primary galaxy are estimated
to quantify the effects of the local and LSS environments. We also define the
projected number density parameter at the 5 nearest neighbour to
characterise the LSS around the CIG galaxies. Out of the 386 CIG galaxies
considered in this study, at least 340 (88\% of the sample) have no physically
linked satellite. Out of the 386 CIG galaxies, 327 (85\% of the sample) have no
physical companion within a projected distance of 0.3 Mpc. The CIG galaxies are
distributed following the LSS of the local Universe, although presenting a
large heterogeneity in their degree of connection with it. A clear segregation
appears between early-type CIG galaxies with companions and isolated late-type
CIG galaxies. Isolated galaxies are in general bluer, with likely younger
stellar populations and rather high star formation with respect to older,
redder CIG galaxies with companions. Reciprocally, the satellites are redder
and with an older stellar populations around massive early-type CIG galaxies,
while they have a younger stellar content around massive late-type CIG
galaxies. This suggests that the CIG is composed of a heterogeneous population
of galaxies, sampling from old to more recent, dynamical systems of galaxies.Comment: 19 pages, 10 figures, 1 table, accepted for publication in Astronomy
& Astrophysic
SDSS IV MaNGA: Dependence of Global and Spatially Resolved SFR-M ∗ Relations on Galaxy Properties
Indexación: Scopus.The galaxy integrated Hα star formation rate-stellar mass relation, or SFR(global)-M ∗(global) relation, is crucial for understanding star formation history and evolution of galaxies. However, many studies have dealt with SFR using unresolved measurements, which makes it difficult to separate out the contamination from other ionizing sources, such as active galactic nuclei and evolved stars. Using the integral field spectroscopic observations from SDSS-IV MaNGA, we spatially disentangle the contribution from different Hα powering sources for ∼1000 galaxies. We find that, when including regions dominated by all ionizing sources in galaxies, the spatially resolved relation between Hα surface density (ΣHα(all)) and stellar mass surface density (Σ∗(all)) progressively turns over at the high Σ∗(all) end for increasing M ∗(global) and/or bulge dominance (bulge-to-total light ratio, B/T). This in turn leads to the flattening of the integrated Hα(global)-M ∗(global) relation in the literature. By contrast, there is no noticeable flattening in both integrated Hα(H ii)-M ∗(H ii) and spatially resolved ΣHα(H ii)-Σ∗(H ii) relations when only regions where star formation dominates the ionization are considered. In other words, the flattening can be attributed to the increasing regions powered by non-star-formation sources, which generally have lower ionizing ability than star formation. An analysis of the fractional contribution of non-star-formation sources to total Hα luminosity of a galaxy suggests a decreasing role of star formation as an ionizing source toward high-mass, high-B/T galaxies and bulge regions. This result indicates that the appearance of the galaxy integrated SFR-M ∗ relation critically depends on their global properties (M ∗(global) and B/T) and relative abundances of various ionizing sources within the galaxies.http://iopscience.iop.org/article/10.3847/1538-4357/aaa9bc/met
SIT 45: An interacting, compact, and star-forming isolated galaxy triplet
The merging system SIT 45 (UGC 12589) is an unusual isolated galaxy triplet,
consisting of three merging late-type galaxies, out of 315 systems in the SIT
(SDSS-based catalogue of Isolated Triplets). The main aims of this work are to
study its dynamical evolution and star formation history (SFH), as well as its
dependence on its local and large-scale environment. To study its dynamics,
parameters such as the velocity dispersion (), the harmonic radius
(), the crossing time (), and the virial mass (), along
with the compactness of the triplet () were considered. To constrain the
SFH, we used CIGALE to fit its observed spectral energy distribution using
multi-wavelength data from the ultraviolet to the infrared. According to its
SFH, SIT 45 presents star-formation, where the galaxies also present recent
(200 Myr) star-formation increase, indicating that this activity may
have been triggered by the interaction. Its dynamical configuration suggests
that the system is highly evolved in comparison to the SIT. However this is not
expected for systems composed of star-forming late-type galaxies, based on
observations in compact groups. We conclude that SIT 45 is a system of three
interacting galaxies that are evolving within the same dark matter halo, where
its compact configuration is a consequence of the on-going interaction, rather
than due to a long-term evolution (as suggested from its value). We
consider two scenarios for the present configuration of the triplet, one where
one of the members is a tidal galaxy, and another where this galaxy arrives to
the system after the interaction. Both scenarios need further exploration. The
isolated triplet SIT 45 is therefore an ideal system to study short timescale
mechanisms ( years), such as starbursts triggered by interactions
which are more frequent at higher redshift.Comment: 13 pages, 7 figures, accepted for publication in Astronomy &
Astrophysic
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Evidence for the Accretion of Gas in Star-forming Galaxies: High N/O Abundances in Regions of Anomalously Low Metallicity
While all models for the evolution of galaxies require the accretion of gas to sustain their growth via on-going star formation, it has proven difficult to directly detect this inflowing material. In this paper we use data of nearby star-forming galaxies in the SDSS IV Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey to search for evidence of accretion imprinted in the chemical composition of the interstellar medium. We measure both the O/H and N/O abundance ratios in regions previously identified as having anomalously low values of O/H. We show that the unusual locations of these regions in the N/O vs. O/H plane indicate that they have been created through the mixing of disk gas having higher metallicity with accreted gas having lower metallicity. Taken together with previous analysis on these anomalously low-metallicity regions, these results imply that accretion of metal-poor gas can probably sustain star formation in present-day late-type galaxies.ERC
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Long-term follow-up of prophylactic mesh reinforcement after emergency laparotomy. A retrospective controlled study
Prevention of incisional hernias with a prophylactic mesh in emergency surgery is controversial. The present study aimed to analyze the long-term results of prophylactic mesh used for preventing incisional hernia after emergency midline laparotomies. This study was a registered (NCT04578561) retrospective analysis of patients who underwent an emergency midline laparotomy between January 2009 and July 2010 with a follow-up period of longer than 2 years. Long-term outcomes and risk factors for the development of incisional hernias between patients who received a prophylactic reinforcement mesh (Group M) and suture (Group S) were compared. From an initial 266 emergency midline laparotomies, 187 patients were included. The median follow-up time was 64.4 months (SD 35). Both groups had similar characteristics, except for a higher rate of previous operations (62 vs. 43.2%; P = 0.01) and operation due to a revision laparotomy (32.5 vs.13%; P = 0.02) in the M group. During follow-up, 29.9% of patients developed an incisional hernia (Group S 36.6% vs. Group M 14.3%; P = 0.002). Chronic mesh infections were diagnosed in 2 patients, but no mesh explants were needed, and no patient in the M group developed chronic pain. Long-term risk factors for incisional hernia were as follows: smoking (HR = 2.47; 95% CI 1.318-4.624; P = 0.05), contaminated surgery (HR = 2.98; 95% CI 1.142-7.8; P = 0.02), surgical site infection (SSI; HR = 3.83; 95% CI 1.86-7.86; P = 0.001), and no use of prophylactic mesh (HR = 5.09; 95% CI 2.1-12.2; P = 0.001). Incidence of incisional hernias after emergency midline laparotomies is high and increases with time. High-risk patients, contaminated surgery, and surgical site infection (SSI) benefit from mesh reinforcement. Prophylactic mesh use is safe and feasible in emergencies with a low long-term complication rate. Trial registration: NCT04578561
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