2,972 research outputs found
PMAS: The Potsdam Multi Aperture Spectrophotometer. II. The Wide Integral Field Unit PPak
PPak is a new fiber-based Integral Field Unit (IFU), developed at the
Astrophysical Institute Potsdam, implemented as a module into the existing PMAS
spectrograph. The purpose of PPak is to provide both an extended field-of-view
with a large light collecting power for each spatial element, as well as an
adequate spectral resolution. The PPak system consists of a fiber bundle with
331 object, 36 sky and 15 calibration fibers. The object and sky fibers collect
the light from the focal plane behind a focal reducer lens. The object fibers
of PPak, each 2.7 arcseconds in diameter, provide a contiguous hexagonal
field-of-view of 74 times 64 arcseconds on the sky, with a filling factor of
60%. The operational wavelength range is from 400 to 900nm. The PPak-IFU,
together with the PMAS spectrograph, are intended for the study of extended,
low surface brightness objects, offering an optimization of total
light-collecting power and spectral resolution. This paper describes the
instrument design, the assembly, integration and tests, the commissioning and
operational procedures, and presents the measured performance at the telescope.Comment: 14 pages, 21 figures, accepted at PAS
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The CALIFA Survey: Exploring the Oxygen Abundance in the Local Universe
We present here a review of the latest results on the spatially-resolved analysis of the stellar populations and ionized gas of disk-dominated galaxies based on Calar Alto Legacy Integral Field Area (CALIFA) data. CALIFA is an ongoing integral field spectroscopy (IFS) survey of galaxies in the Local Universe (0.005 2 re; and (iii) an inner drop at <0.5 re that depends on mass; (4) the presence of bending in the surface brightness profile of disk galaxies is not clearly related to either the change in the shape of the oxygen abundance profile or the properties of the underlying stellar population. All of these results indicate that disk galaxies present an overall inside-out growth, with chemical enrichment and stellar mass growth tightly correlated and dominated by local processes and limited effects of radial mixing or global outflows. However, clear deviations are shown with respect to this simple scenario, which affect the abundance profiles in both the innermost and outermost regions of galaxie
A Local Leaky-Box Model for the Local Stellar Surface Density-Gas Surface Density-Gas Phase Metallicity Relation
We revisit the relation between the stellar surface density, the gas surface density and the gas-phase metallicity of typical disc galaxies in the local Universe with the SDSS-IV/MaNGA survey, using the star formation rate surface density as an indicator for the gas surface density. We show that these three local parameters form a tight relationship, confirming previous works (e.g. by the PINGS and CALIFA surveys), but with a larger sample. We present a new local leaky-box model, assuming star-formation history and chemical evolution is localized except for outflowing materials. We derive closed-form solutions for the evolution of stellar surface density, gas surface density and gas-phase metallicity, and show that these parameters form a tight relation independent of initial gas density and time. We show that, with canonical values of model parameters, this predicted relation match the observed one well. In addition, we briefly describe a pathway to improving the current semi-analytic models of galaxy formation by incorporating the local leaky-box model in the cosmological context, which can potentially explain simultaneously multiple properties of Milky Way-type disc galaxies, such as the size growth and the global stellar mass–gas metallicity relation
A Local Leaky-Box Model for the Local Stellar Surface Density-Gas Surface Density-Gas Phase Metallicity Relation
We revisit the relation between the stellar surface density, the gas surface density and the gas-phase metallicity of typical disc galaxies in the local Universe with the SDSS-IV/MaNGA survey, using the star formation rate surface density as an indicator for the gas surface density. We show that these three local parameters form a tight relationship, confirming previous works (e.g. by the PINGS and CALIFA surveys), but with a larger sample. We present a new local leaky-box model, assuming star-formation history and chemical evolution is localized except for outflowing materials. We derive closed-form solutions for the evolution of stellar surface density, gas surface density and gas-phase metallicity, and show that these parameters form a tight relation independent of initial gas density and time. We show that, with canonical values of model parameters, this predicted relation match the observed one well. In addition, we briefly describe a pathway to improving the current semi-analytic models of galaxy formation by incorporating the local leaky-box model in the cosmological context, which can potentially explain simultaneously multiple properties of Milky Way-type disc galaxies, such as the size growth and the global stellar mass–gas metallicity relation
The Recent Star Formation History of NGC 5102
We present Hubble Space Telescope photometry of young stars in NGC 5102, a
nearby gas-rich post-starburst S0 galaxy with a bright young stellar nucleus.
We use the IAC-pop/MinnIAC algorithm to derive the recent star formation
history in three fields in the bulge and disk of NGC 5102. In the disk fields,
the recent star formation rate has declined monotonically and is now barely
detectable, but a starburst is still in progress in the bulge and has added
about 2 percent to the mass of the bulge over the last 200 Myr. Other studies
of star formation in NGC 5102 indicate that about 20 percent of its stellar
mass was added over the past Gyr. If this is correct, then much of the stellar
mass of the bulge may have formed over this period. It seems likely that this
star formation was fueled by the accretion of a gas-rich system with HI mass of
about 2 x 10^9 Msol which has now been almost completely converted into stars.
The large mass of recently formed stars and the blue colours of the bulge
suggest that the current starburst, which is now fading, may have made a
significant contribution to build the bulge of NGC 5102.Comment: 36 pages, 16 figures, accepted in A
Optically-passive spirals: The missing link in gradual star formation suppression upon cluster infall
Galaxies migrate from the blue cloud to the red sequence when their star
formation is quenched. Here, we report on galaxies quenched by environmental
effects and not by mergers or strong AGN as often invoked: They form stars at a
reduced rate which is optically even less conspicuous, and manifest a
transition population of blue spirals evolving into S0 galaxies. These
'optically passive' or 'red spirals' are found in large numbers in the STAGES
project (and by Galaxy Zoo) in the infall region of clusters and groups.Comment: Proceedings of "The Starburst-AGN connection" conference held in
Shanghai, Oct 27-31, 200
Spatial metallicity distribution statistics at pc scales in the AMUSING++ nearby galaxy sample
We analyse the spatial statistics of the 2D gas-phase oxygen abundance
distributions in a sample of 219 local galaxies. We introduce a new adaptive
binning technique to enhance the signal-to-noise ratio of weak lines, which we
use to produce well-filled metallicity maps for these galaxies. We show that
the two-point correlation functions computed from the metallicity distributions
after removing radial gradients are in most cases well described by a simple
injection-diffusion model. Fitting the data to this model yields the
correlation length , which describes the characteristic
interstellar medium mixing length scale. We find typical correlation lengths
kpc, with a strong correlation between and
stellar mass, star formation rate, and effective radius, a weak correlation
with Hubble type, and significantly elevated values of in
interacting or merging galaxies. We show that the trend with star formation
rate can be reproduced by a simple transport+feedback model of interstellar
medium turbulence at high star formation rate, and plausibly also at low star
formation rate if dwarf galaxy winds have large mass-loading factors. We also
report the first measurements of the injection width that describes the initial
radii over which supernova remnants deposit metals. Inside this radius the
metallicity correlation function is not purely the product of a competition
between injection and diffusion. We show that this size scale is generally
smaller than 60 pc.Comment: 18 pages, 18 figures, 1 table, submitted to MNRAS. Comments are
welcom
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