95 research outputs found
Gravitational Potential and Surface Density Drive Stellar Populations -- II. Star-Forming Galaxies
Stellar population parameters correlate with a range of galaxy properties,
but it is unclear which relations are causal and which are the result of
another underlying trend. In this series, we quantitatively compare trends
between stellar population properties and galaxy structural parameters in order
to determine which relations are intrinsically tighter, and are therefore more
likely to reflect a causal relation. Specifically, we focus on the galaxy
structural parameters of mass , gravitational potential ,
and surface mass density . In Barone et al. (2018) we found
that for early-type galaxies the age- and [Z/H]- relations show
the least intrinsic scatter as well as the least residual trend with galaxy
size. In this work we study the ages and metallicities measured from full
spectral fitting of 2085 star-forming galaxies from the SDSS Legacy Survey,
selected so all galaxies in the sample are probed to one effective radius. As
with the trends found in early-type galaxies, we find that in star-forming
galaxies age correlates best with stellar surface mass density, and [Z/H]
correlates best with gravitational potential. We discuss multiple mechanisms
that could lead to these scaling relations. For the [Z/H]-- relation we
conclude that gravitational potential is the primary regulator of metallicity,
via its relation to the gas escape velocity. The age-- relation is
consistent with compact galaxies forming earlier, as higher gas fractions in
the early universe cause old galaxies to form more compactly during their
in-situ formation phase, and may be reinforced by compactness-related quenching
mechanisms.Comment: Accepted for publication in ApJ. 20 pages, 9 figures, 1 tabl
Ultraluminous Quasars At High Redshift Show Evolution In Their Radio-Loudness Fraction In Both Redshift And Ultraviolet Luminosity
We take a sample of 94 ultraluminous, optical quasars from the search of over
14,486 deg^2 by Onken et al. 2022 in the range 4.4<redshift<5.2 and match them
against the Rapid ASKAP Continuum Survey (RACS) observed on the Australian
Square Kilometre Array Pathfinder (ASKAP). From this most complete sample of
the bright end of the redshift ~5 quasar luminosity function, there are 10
radio continuum detections of which 8 are considered radio-loud quasars. The
radio-loud fraction for this sample is 8.5 \pm 2.9 per cent. Jiang et al. 2007
found that there is a decrease in the radio-loud fraction of quasars with
increasing redshift and an increase with increasing absolute magnitude at rest
frame 2500 Angstroms. We show that the radio-loud fraction of our quasar sample
is consistent with that predicted by Jiang et al. 2007, extending their result
to higher redshifts.Comment: Accepted by MNRA
On the distribution of galaxy ellipticity in clusters
We study the distribution of projected ellipticity n(ϵ) for galaxies in a sample of 20 rich (Richness ≥ 2) nearby (z 0.4), therefore it is not a consequence of the increasing fraction of round slow rotator galaxies near cluster centers. Furthermore, the ϵ-R relation persists for just smooth flattened galaxies and for galaxies with de Vaucouleurs-like light profiles, suggesting that the variation of the spiral fraction with radius is not the underlying cause of the trend. We interpret our findings in light of the classification of early type galaxies (ETGs) as fast and slow rotators. We conclude that the observed trend of decreasing ϵ towards the centres of clusters is evidence for physical effects in clusters causing fast rotator ETGs to have a lower average intrinsic ellipticity near the centres of rich clusters
The gas-phase metallicities of star-forming galaxies in aperture-matched SDSS samples follow potential rather than mass or average surface density
We present a comparative study of the relation between the aperture-based
gas-phase metallicity and three structural parameters of star-forming galaxies:
mass (), average potential () and average surface mass density (; where is the effective radius). We use a
volume-limited sample drawn from the publicly available SDSS DR7, and base our
analysis on aperture-matched sampling by selecting sets of galaxies where the
SDSS fibre probes a fixed fraction of . We find that between 0.5
and 1.5 , the gas-phase metallicity correlates more tightly with
than with either or , in that for all
aperture-matched samples, the potential-metallicity relation has (i) less
scatter, (ii) higher Spearman rank correlation coefficient and (iii) less
residual trend with than either the mass-metallicity relation
and the average surface density-metallicity relation. Our result is broadly
consistent with the current models of gas enrichment and metal loss. However, a
more natural explanation for our findings is a local relation between the
gas-phase metallicity and escape velocity.Comment: Accepted by MNRAS; 17 pages, 11 figures, 1 tabl
On the distribution of galaxy ellipticity in clusters
open4We study the distribution of projected ellipticity n(ε) for galaxies in a sample of 20 rich (Richness ≥ 2) nearby (z 0.4), therefore it is not a consequence of the increasing fraction of round slow rotator galaxies near cluster centers. Furthermore, the ε-R relation persists for just smooth flattened galaxies and for galaxies with deVaucouleurs-like light profiles, suggesting that the variation of the spiral fractionwith radius is not the underlying cause of the trend. We interpret our findings in light of the classification of early type galaxies (ETGs) as fast and slow rotators. We conclude that the observed trend of decreasing ε towards the centres of clusters is evidence for physical effects in clusters causing fast rotator ETGs to have a lower average intrinsic ellipticity near the centres of rich clusters.openD'Eugenio F.; Houghton R.C.W.; Davies R.L.; Dalla Bonta' E.D'Eugenio, F.; Houghton, R. C. W.; Davies, R. L.; Dalla Bonta', E
SHDE: Survey description and mass-kinematics scaling relations for dwarf galaxies
The Study of H from Dwarf Emissions (SHDE) is a high spectral
resolution (R=13500) H integral field survey of 69 dwarf galaxies with
stellar masses . The survey used FLAMES on
the ESO Very Large Telescope. SHDE is designed to study the kinematics
and stellar populations of dwarf galaxies using consistent methods applied to
massive galaxies and at matching level of detail, connecting these mass ranges
in an unbiased way. In this paper we set out the science goals of SHDE,
describe the sample properties, outline the data reduction and analysis
processes. We investigate the mass-kinematics
scaling relation, which have previously shown potential for combining galaxies
of all morphologies in a single scaling relation. We extend the scaling
relation from massive galaxies to dwarf galaxies, demonstrating this relation
is linear down to a stellar mass of .
Below this limit, the kinematics of galaxies inside one effective radius appear
to be dominated by the internal velocity dispersion limit of the
H-emitting gas, giving a bend in the
relation. Replacing stellar mass with total baryonic mass using gas mass
estimate reduces the severity but does not remove the linearity limit of the
scaling relation. An extrapolation to estimate the galaxies' dark matter halo
masses, yields a scaling relation that is free of
any bend, has reduced curvature over the whole mass range, and brings galaxies
of all masses and morphologies onto the virial relation.Comment: 19 pages, 13 figures, 5 tables; published in MNRA
Galaxy And Mass Assembly (GAMA): Stellar-to-Dynamical Mass Relation I. Constraining the Precision of Stellar Mass Estimates
In this empirical work, we aim to quantify the systematic uncertainties in
stellar mass estimates made from spectral energy distribution (SED)
fitting through stellar population synthesis (SPS), for galaxies in the local
Universe, by using the dynamical mass estimator as an
SED-independent check on stellar mass. We first construct a statistical model
of the high dimensional space of galaxy properties; size , velocity
dispersion , surface brightness , mass-to-light ratio
, rest-frame colour, S\'ersic index and dynamical mass
; accounting for selection effects and covariant errors. We
disentangle the correlations among galaxy properties and find that the
variation in is driven by , S\'ersic index and
colour. We use these parameters to calibrate an SED-independent
estimator, . We find the random scatter of the relation
to be and for
quiescent and star-forming galaxies respectively. Finally, we inspect the
residuals as a function of SPS parameters (dust, age, metallicity, star
formation rate) and spectral indices (H, H, . For
quiescent galaxies, of the scatter can be explained by the
uncertainty in SPS parameters, with dust and age being the largest sources of
uncertainty. For star-forming galaxies, while age and metallicity are the
leading factors, SPS parameters account for only of the scatter.
These results leave us with remaining unmodelled scatters of
and for quiescent and star-forming galaxies respectively.
This can be interpreted as a conservative limit on the precision in
that can be achieved via simple SPS-modelling.Comment: Accepted for publication in the Astrophysical Journal on 14 June 202
Comparison of the Stellar Populations of Bulges and Discs using the MaNGA Survey
We use the MaNGA integral-field spectroscopic survey of low-redshift galaxies
to compare the stellar populations of the bulge and disc components, identified
from their Sersic profiles, for various samples of galaxies. Bulge dominated
regions tend to be more metal-rich and have slightly older stellar ages than
their associated disc dominated regions. The metallicity difference is
consistent with the deeper gravitational potential in bulges relative to discs,
which allows bulges to retain more of the metals produced by stars. The age
difference is due to star formation persisting longer in discs relative to
bulges. Relative to galaxies with lower stellar masses, galaxies with higher
stellar masses tend to have bulge dominated regions that are more metal-rich
and older (in light-weighted measurements) than their disc dominated regions.
This suggests high-mass galaxies quench from the inside out, while lower-mass
galaxies quench across the whole galaxy simultaneously. Early-type galaxies
tend to have bulge dominated regions the same age as their disc dominated
regions, while late-type galaxies tend to have disc dominated regions
significantly younger than their bulge dominated regions. Central galaxies tend
to have a greater metallicity difference between their bulge dominated regions
and disc dominated regions than satellite galaxies at similar stellar mass.
This difference may be explained by central galaxies being subject to mergers
or extended gas accretion bringing new, lower-metallicity gas to the disc,
thereby reducing the average metallicity and age of the stars; quenching of
satellite discs may also play a role.Comment: Accepted by PAS
The black hole mass metallicity relation and insights into galaxy quenching
One of the most important questions in astrophysics is what causes galaxies
to stop forming stars. Previous studies have shown a tight link between
quiescence and black hole mass. Other studies have revealed that quiescence is
also associated with 'starvation', the halting of gas inflows, which results in
the remaining gas being used up rapidly by star formation and in rapid chemical
enrichment. In this work we find the final missing link between these two
findings. Using a large sample of galaxies, we uncover the intrinsic
dependencies of the stellar metallicity on galaxy properties. In the case of
the star-forming galaxies, the stellar metallicity is driven by stellar mass.
However, for passive galaxies the stellar metallicity is primarily driven by
the black hole mass, as traced by velocity dispersion. This result finally
reveals the connection between previous studies, where the integrated effect of
black hole feedback prevents gas inflows, starving the galaxy, which is seen by
the rapid increase in the stellar metallicity, leading to the galaxy becoming
passive.Comment: 20 pages, 6 figures, submitted to Nature Astronom
Stars, gas, and star formation of distant post-starburst galaxies
We present a comprehensive multi-wavelength study of 5 poststarburst galaxies
with at , examining their stars, gas, and
current and past star-formation activities. Using optical images from the
Subaru telescope and Hubble Space Telescope, we observe a high incidence of
companion galaxies and low surface brightness tidal features, indicating that
quenching is closely related to interactions between galaxies. From optical
spectra provided by the LEGA-C survey, we model the stellar continuum to derive
the star-formation histories and show that the stellar masses of progenitors
ranging from to , undergoing a burst of
star formation several hundred million years prior to observation, with a decay
time scale of million years. Our ALMA observations detect CO(2-1)
emission in four galaxies, with the molecular gas spreading over up to ,
or kpc, with a mass of up to . However,
star-forming regions are unresolved by either the slit spectra or 3~GHz
continuum observed by the Very Large Array. Comparisons between the
star-formation rates and gas masses, and the sizes of CO emission and
star-forming regions suggest a low star-forming efficiency. We show that the
star-formation rates derived from IR and radio luminosities with commonly-used
calibrations tend to overestimate the true values because of the prodigious
amount of radiation from old stars and the contribution from AGN, as the
optical spectra reveal weak AGN-driven outflows.Comment: Accepted by Ap
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