J. C. Muñoz-Mateos

European Southern Observatory, Arching, Bavaria, Germany

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Publications (44)102.74 Total impact

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    ABSTRACT: Using 3.6$\mu$m images of 97 early-type galaxies, we develop and verify methodology to measure globular cluster populations from the S$^4$G survey images. We find that 1) the ratio, T$_{\rm N}$, of the number of clusters, N$_{\rm CL}$, to parent galaxy stellar mass, M$_*$, rises weakly with M$_*$ for early-type galaxies with M$_* > 10^{10}$ M$_\odot$ when we calculate galaxy masses using a universal stellar initial mass function (IMF), but that the dependence of T$_{\rm N}$ on M$_*$ is removed entirely once we correct for the recently uncovered systematic variation of IMF with M$_*$, and 2) for M$_* < 10^{10}$ M$_\odot$ there is no trend between N$_{\rm CL}$ and M$_*$, the scatter in T$_{\rm N}$ is significantly larger (approaching 2 orders of magnitude), and there is evidence to support a previous, independent suggestion of two families of galaxies. The behavior of N$_{\rm CL}$ in the lower mass systems is more difficult to measure because these systems are inherently cluster poor, but our results may add to previous evidence that large variations in cluster formation and destruction efficiencies are to be found among low mass galaxies. The average fraction of stellar mass in clusters is $\sim$ 0.0014 for M$_* > 10^{10}$ M$_\odot$ and can be as large as $\sim 0.02$ for less massive galaxies. These are the first results from the S$^4$G sample of galaxies, and will be enhanced by the sample of early-type galaxies now being added to S$^4$G and complemented by the study of later type galaxies within S$^4$G.
    11/2014;
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    ABSTRACT: The mid-infrared is an optimal window to trace stellar mass in nearby galaxies and the 3.6 micron IRAC band has been exploited to this effect, but such mass estimates can be biased by dust emission. We present our pipeline to reveal the old stellar flux at 3.6 micron and obtain stellar mass maps for more than 1600 galaxies available from the Spitzer Survey of Stellar Structure in Galaxies (S4G). This survey consists of images in two infrared bands (3.6 and 4.5 micron), and we use the Independent Component Analysis (ICA) method presented in Meidt et al. (2012) to separate the dominant light from old stars and the dust emission that can significantly contribute to the observed 3.6 micron flux. We exclude from our ICA analysis galaxies with low signal-to-noise (S/N < 10) and those with original [3.6]-[4.5] colors compatible with an old stellar population, indicative of little dust emission (mostly early Hubble types, which can directly provide good mass maps). For the remaining 1251 galaxies to which ICA was successfully applied, we find that as much as 10-30% of the total light at 3.6 micron typically originates from dust, and locally it can reach even higher values. This contamination fraction shows a correlation with specific star formation rates, confirming that the dust emission that we detect is related to star formation. Additionally, we have used our large sample of mass estimates to calibrate a relationship of effective M/L as a function of observed [3.6]-[4.5] color: log(M/L)=-0.339 (+/- 0.057) x ([3.6]-[4.5]) -0.336 (+/-0.002). Our final pipeline products will be made public through IRSA, providing the astronomical community with an unprecedentedly large set of stellar mass maps ready to use for scientific applications.
    09/2014;
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    ABSTRACT: Physical conditions of the interstellar medium in galaxies are closely linked to the ambient radiation field and the heating of dust grains. In order to characterize dust properties in galaxies over a wide range of physical conditions, we present here the radial surface brightness profiles of the entire sample of 61 galaxies from Key Insights into Nearby Galaxies: Far-Infrared Survey with Herschel (KINGFISH). The main goal of our work is the characterization of the grain emissivities, dust temperatures, and interstellar radiation fields responsible for heating the dust. After fitting the dust and stellar radial profiles with exponential functions, we fit the far-infrared spectral energy distribution (SED) in each annular region with single-temperature modified black bodies using both variable (MBBV) and fixed (MBBF) emissivity indices beta, as well as with physically motivated dust models. Results show that while most SED parameters decrease with radius, the emissivity index beta also decreases with radius in some galaxies, but in others is increasing, or rising in the inner regions and falling in the outer ones. Despite the fixed grain emissivity (average beta~ 2.1) of the physically-motivated models, they are well able to accommodate flat spectral slopes with beta<= 1. We find that flatter slopes (beta<= 1.5) are associated with cooler temperatures, contrary to what would be expected from the usual Tdust-beta degeneracy. This trend is related to variations in Umin since beta and Umin are very closely linked over the entire range in Umin sampled by the KINGFISH galaxies: low Umin is associated with flat beta<=1. Both these results strongly suggest that the low apparent \beta values (flat slopes) in MBBV fits are caused by temperature mixing along the line-of-sight, rather than by intrinsic variations in grain properties. Abstract truncated for arXiv.
    09/2014;
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    ABSTRACT: We study the surface brightness profiles of disc galaxies in the 3.6 micron images from the Spitzer Survey of Stellar Structure in Galaxies (S4G) and K_s-band images from the Near Infrared S0-Sa galaxy Survey (NIRS0S). We particularly connect properties of single exponential (type I), downbending double exponential (type II), and upbending double exponential (type III) disc profile types, to structural components of galaxies by using detailed morphological classifications, and size measurements of rings and lenses. We also study how the local environment of the galaxies affects the profile types by calculating parameters describing the environmental density and the tidal interaction strength. We find that in majority of type II profiles the break radius is connected with structural components such as rings, lenses, and spirals. The exponential disc sections of all three profile types, when considered separately, follow the disc scaling relations. However, the outer discs of type II, and the inner discs of type III, are similar in scalelength to the single exponential discs. Although the different profile types have similar mean environmental parameters, the scalelengths of the type III profiles show a positive correlation with the tidal interaction strength.
    04/2014; 441(3).
  • A. Y. K. Bouquin, A. Gil de Paz, S. Boissier, J. C. Muñoz-Mateos
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    ABSTRACT: We have obtained GALEX UV radial surface brightness and color profiles, as well as integrated magnitudes for +1500 galaxies covering ̃70% of the S4G/DAGAL volume-limited sample of nearby galaxies (d < 40Mpc), and combined these with S4G Spitzer/IRAC-3.6 μm photometry. The analysis of the (FUV-NUV) vs. (NUV-[3.6]) color-color and (FUV-NUV) vs. M[3.6] color-magnitude diagrams (CMD) reveal both a narrow so-called “blue sequence”, where Irr through Sb's are located, and a “red cloud”, where E/S0 galaxies reside. This is opposite to the morphology seen in optical CMDs, and in the case of the color-color diagram, it reflects the degeneracy between SFH of disk galaxies and dust extinction (which strongly correlates the FUV-NUV and NUV-[3.6] colors) and could only be seen in its full extent thanks to the statistics and wide range of galaxy masses and types provided by S4G/DAGAL. We find that a large fraction (%) of the galaxies evolving off (or into) this “blue sequence” towards (or from) the “red cloud” are early-type spirals, that we interpret as a sign of strangulation (or re-birth) of the star formation in these galaxies. Such processes lead to distinct FUV-NUV colors, as this color is very sensitive to recent changes in the star formation activity, compared to other colors (optical ones, NUV-optical, or even NUV-[3.6]).
    02/2014;
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    ABSTRACT: We present Herschel/PACS 100 and 160 micron integrated photometry for the 323 galaxies in the Herschel Reference Survey (HRS), a K-band-, volume-limited sample of galaxies in the local Universe. Once combined with the Herschel/SPIRE observations already available, these data make the HRS the largest representative sample of nearby galaxies with homogeneous coverage across the 100-500 micron wavelength range. In this paper, we take advantage of this unique dataset to investigate the properties and shape of the far-infrared/sub-millimeter spectral energy distribution in nearby galaxies. We show that, in the stellar mass range covered by the HRS (8<log(M*/Msun)<12), the far-infrared/sub-millimeter colours are inconsistent with a single modified black-body having the same dust emissivity index beta for all galaxies. In particular, either beta decreases, or multiple temperature components are needed, when moving from metal-rich/gas-poor to metal-poor/gas-rich galaxies. We thus investigate how the dust temperature and mass obtained from a single modified black-body depend on the assumptions made on beta. We show that, while the correlations between dust temperature, galaxy structure and star formation rate are strongly model dependent, the dust mass scaling relations are much more reliable, and variations of beta only change the strength of the observed trends.
    02/2014; 440(1).
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    ABSTRACT: The study of early type galaxies (ellipticals and lenticulars) is undergoing a renaissance with new observations that are confronting our notions of these systems as being old, dead and red. Observations are revealing stellar substructure, gas and dust, star formation and tidal debris in these galaxies, all of which are challenging our understanding of the formation and evolution of these 'simple' systems. Here we propose to assemble a complete survey of all nearby early type galaxies (ETGs) using archival and new observations for all ETGs at d < 40 Mpc (v < 3000.0 km/s), m_B < 15.5, D_25 > 1 arcminute and \|b\| > 30 degrees. We request 188.1 hrs to map 465 ETGs at 3.6 and 4.5 microns - this will provide a statistically robust and complete sample of ETGs with sufficient numbers in each mass, type and environment to study their structure, reconstruct their evolution through stellar populations, assess their recent merger history and ultimately constrain their origins. These data will be the most sensitive probe to date for faint stellar structures such as nuclear cusps, large scale shells and rings, and stellar disks in the largest sample of ETGs ever assembled, providing an extremely sensitive test of current and future models for the formation and evolution of ETGs over cosmic time.
    Spitzer Proposal. 10/2013;
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    ABSTRACT: We study the m=1 distortions (lopsidedness) in the stellar components of 167 nearby galaxies that span a wide range of morphologies and luminosities. We confirm the previous findings of 1) a high incidence of lopsidedness in the stellar distributions, 2) increasing lopsidedness as a function of radius out to at least 3.5 exponential scale lengths, and 3) greater lopsidedness, over these radii, for galaxies of later type and lower surface brightness. Additionally, the magnitude of the lopsidedness 1) correlates with the character of the spiral arms (stronger arm patterns occur in galaxies with less lopsidedness), 2) is not correlated with the presence or absence of a bar, or the strength of the bar when one is present, 3) is inversely correlated to the stellar mass fraction, f_*, within one radial scale length, and 4) correlates directly with f_* measured within the radial range over which we measure lopsidedness. We interpret these findings to mean that lopsidedness is a generic feature of galaxies and does not, generally, depend on a rare event, such as a direct accretion of a satellite galaxy onto the disk of the parent galaxy. While lopsidedness may be caused by several phenomena, moderate lopsidedness ( _i + _o)/2 < 0.3) is likely to reflect halo asymmetries to which the disk responds or a gravitationally self-generated mode . We hypothesize that the magnitude of the stellar response depends both on how centrally concentrated the stars are with respect to the dark matter and whether there are enough stars in the region of the lopsidedness that self-gravity is dynamically important.
    The Astrophysical Journal 05/2013; 772(2). · 6.73 Impact Factor
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    ABSTRACT: MEGARA (Multi-Espectrógrafo en GTC de Alta Resolución para Astronomía) is an optical Integral-Field Unit (IFU) and Multi-Object Spectrograph (MOS) designed for the GTC 10.4 m telescope in La Palma. MEGARA will be a 3rd generation instrument for GTC. It is led by the University Complutense of Madrid with the collaboration of INAOE, IAA, UPM and comprises more than 50 researchers from a large number of institutions worldwide.
    05/2013;
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    ABSTRACT: Local Luminous Compact Blue Galaxies (LCBG) are the closest counterpart of the high z outburst population. These objects are crucial as a local reference for compact star-forming galaxies observed at cosmological distances. We have obtained 2-D spectroscopy in the 3700-7000 Å range with PPAK instrument (at 3.5 m CAHA) for a sample of 22 local LCBGs. In this poster we show the results derived from the 2D analysis of different physical properties in UCM1648+2855, a case study LCBG. It was chosen as a prototype of one of the three kinematic classes observed by Pérez-Gallego, et al. (2011): perturbed rotation. Our study shows that this galaxy has a dichotomy between eastern star-forming region and the western part that shows an old underlying stellar population. UCM1648+2855 has a disc-supported velocity map, perturbed by two large star-forming regions; and an enhanced dust distribution outside the star-forming regions. Therefore the massive star formation in UCM1648+2855 seems to be not driven by merging (or any accompanying galaxy), but by a genuine starburst, with a SFR of ˜ 9 {M}_{⊙}/year.
    05/2013;
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    ABSTRACT: Luminous Compact Blue Galaxies (LCBGs) are small, but vigorously star forming galaxies. Their presence at different redshifts denotes their cosmological relevance and implies that local starburst galaxies, when properly selected, are unique laboratories for studying the complex ecosystem of the star formation process over time. We have selected a representative sample of 22 LCBGs from the SDSS and UCM databases which, although small, provides an excellent reference for comparison with current and future surveys of similar starbursts at high-z. We are carrying out a 2D optical spectroscopic study of this LCBG sample, including spatially resolved maps of kinematics, extinction, SFR and metallicity. This will help us to answer questions regarding the nature of these objects. In this poster we show our results on the kinematical study (Pérez-Gallego et al. 2011) which allows us to classify these galaxies into three different classes: rotating disk (RD) 48%, perturbed rotation (PR) 28% and complex kinematics (CK) 24%. We find 5% of objects show evidence of a recent major merger, 10% of a minor merger, and 45% of a companion. This argues in favor of ongoing interactions with close companions as a mechanism for the enhanced star formation activity in these galaxies. We find only 5% of objects with clear evidence of AGN activity, and 27% with kinematics consistent with SN-driven galactic winds. Therefore, a different mechanism may be responsible for quenching the star formation in LCBGs. The detailed analysis of the physical properties for each galaxy in the sample is on progress and we show in this poster the results on UCM2325+2318 as a prototype LCBG. Between the possible mechanisms to explain the starburst activity in this galaxy, our 2D spectroscopic data support the scenario of an on-going interaction with the possibility for clump B to be the dwarf satellite galaxy (Castillo-Morales et al. 2011, Pérez-Gallego et al. 2010).
    05/2013;
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    ABSTRACT: We have analyzed the radial distribution of old stars in a sample of 218 nearby face-on disks, using deep 3.6um images from the Spitzer Survey of Stellar Structure in Galaxies (S4G). In particular, we have studied the structural properties of those disks with a broken or down-bending profile. We find that, on average, disks with a genuine single exponential profile have a scale-length and a central surface brightness which are intermediate to those of the inner and outer components of a down-bending disk with the same total stellar mass. In the case of barred galaxies, the ratio between the break and the bar radii (Rbr/Rbar) depends strongly on the total stellar mass of the galaxy. For galaxies more massive than 10^10 Msun, the distribution is bimodal, peaking at Rbr/Rbar~2 and ~3.5. The first peak, which is the most populated one, is linked to the Outer Lindblad Resonance of the bar, whereas the second one is consistent with a dynamical coupling between the bar and the spiral pattern. For galaxies below 10^10 Msun, breaks are found up to ~10 Rbar, but we show that they could still be caused by resonances given the rising nature of rotation curves in these low-mass disks. While not ruling out star formation thresholds, our results imply that radial stellar migration induced by non-axysymmetric features can be responsible not only for those breaks at 2 Rbar, but also for many of those found at larger radii.
    The Astrophysical Journal 04/2013; 771(1). · 6.73 Impact Factor
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    ABSTRACT: We present a study of the kinematics of the isolated spiral galaxy NGC 864, using Hα Fabry-Perot data obtained with the Galaxy Hα Fabry-Perot System (GHαFaS) instrument at the William Herschel Telescope in La Palma, complemented with images at 3.6 μm, in the R band and in Hα filter, and integral-field spectroscopic data. The resulting data cubes and velocity maps allow the study of the kinematics of the galaxy, including in-depth investigations of the rotation curve, velocity moment maps, velocity residual maps, gradient maps and position-velocity diagrams. We find asymmetries in the velocity field in the bar zone, caused by non-circular motions, probably in response to the potential of the bar. We also find a flat-profile bar, in agreement with the strong bar, with the grand design spiral pattern, and with the gap between the ends of the bar and the start of the spiral arms. We quantify the rate of massive star formation, which is concentrated in the two spiral arms.
    Monthly Notices of the Royal Astronomical Society 12/2012; 427(4):2938-2949. · 5.52 Impact Factor
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    ABSTRACT: NGC 1097 has an extensive, unique network of jet-like extended structures that stretch out for dozens of kiloparsecs. Their origin has remained a mystery for decades. The evidence for their association with the AGN is weak, and the lack of HI emission in the vicinity makes it unlikely that they are the product of tidal interactions or streams off the main disk of the galaxy. Recent modeling has shown that the structures may be the remnants of a dwarf galaxy, though the type of dwarf remains unclear, and such interactions are complicated by the fact that the main spiral has a large bar. We propose Spitzer observations of these features to determine the streams' true extent, to age-date individual structures by focusing on the old stellar population, estimate their masses, and calculate their metallicities. We will use Spitzer's sensitivity and the degeneracy-breaking IRAC colors to unravel the history of this unusual object. This proposal is part of broader studies by members of this team on galaxy outskirts and interactions, including mergers, streams, shells, asymmetries and lopsidedness, all of which contribute to our understanding of galaxy evolution in the nearby Universe.
    Spitzer Proposal. 12/2012;
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    ABSTRACT: We present a study of the kinematics of the isolated spiral galaxy NGC 864, using H{\alpha} Fabry-Perot data obtained with the GH{\alpha}FaS instrument at the William Herschel Telescope in La Palma, complemented with images at 3.6 {\mu}m, in the R band and in H{\alpha} filter, and integral field spectroscopic data. The resulting data cubes and velocity maps allow the study of the kinematics of the galaxy, including in-depth investigations of the rotation curve, velocity moment maps, velocity residual maps, gradient maps and position-velocity diagrams. We find asymmetries in the velocity field in the bar zone, caused by non-circular motions, probably in response to the potential of the bar. We also find a flat-profile bar, in agreement with the strong bar, with the grand design spiral pattern, and with the gap between the ends of the bar and the start of the spiral arms. We quantify the rate of massive star formation, which is concentrated in the two spiral arms.
    08/2012;
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    ABSTRACT: We present the analysis of the full bi-dimensional optical spectral cube of the nearby spiral galaxy NGC 5668, observed with the PPAK IFU at the Calar Alto observatory 3.5m telescope. We make use of broad-band imaging to provide further constraints on the evolutionary history of the galaxy. This dataset will allow us to improve our understanding of the mechanisms that drive the evolution of disks. We investigated the properties of 62 H II regions and concentric rings in NGC 5668 and derived maps in ionized-gas attenuation and chemical (oxygen) abundances. We find that, while inwards of r\,$\sim\,36",\sim$\,4.4kpc\,$\sim$\,0.36\,$(\frac {D_{25}}{2})$ the derived O/H ratio follows the radial gradient typical of spiral galaxies, the abundance gradient beyond r$\sim36"$ flattens out. The analysis of the multi-wavelength surface brightness profiles of NGC 5668 is performed by fitting these profiles with those predicted by chemo-spectrophotometric evolutionary models of galaxy disks. From this, we infer a spin and circular velocity of $\lambda$=0.053 and v$_{c}$=167\,km\,s$^{-1}$, respectively. The metallicity gradient and rotation curve predicted by this best-fitting galaxy model nicely match the values derived from the IFU observations, especially within r\,$\sim36\arcsec$. The same is true for the colors despite of some small offsets and a reddening in the bluest colors beyond that radius. On the other hand, deviations of some of these properties in the outer disk indicate that a secondary mechanism, possibly gas transfer induced by the presence of a young bar, must have played a role in shaping the recent chemical and star formation histories of NGC 5668.
    The Astrophysical Journal 05/2012; 754(1). · 6.73 Impact Factor
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    ABSTRACT: We examine the effect of circumstellar dust extinction on the near-IR (NIR) contribution of asymptotic giant branch (AGB) stars in intermediate-age clusters throughout the disk of M100. For our sample of 17 AGB-dominated clusters we extract optical-to-mid-IR spectral energy distributions (SEDs) and find that NIR brightness is coupled to the mid-IR dust emission in such a way that a significant reduction of AGB light, of up to 1 mag in the K band, follows from extinction by the dust shell formed during this stage. Since the dust optical depth varies with AGB chemistry (C-rich or O-rich), our results suggest that the contribution of AGB stars to the flux from their host clusters will be closely linked to the metallicity and the progenitor mass of the AGB star, to which dust chemistry and mass-loss rate are sensitive. Our sample of clusters-each the analogue of a {approx}1 Gyr old post-starburst galaxy-has implications within the context of mass and age estimation via SED modeling at high-z: we find that the average {approx}0.5 mag extinction estimated here may be sufficient to reduce the AGB contribution in the (rest-frame) K band from {approx}70%, as predicted in the latest generation of synthesis models, to {approx}35%. Our technique for selecting AGB-dominated clusters in nearby galaxies promises to be effective for discriminating the uncertainties associated with AGB stars in intermediate-age populations that plague age and mass estimation in high-z galaxies.
    The Astrophysical Journal Letters 04/2012; 748:L30. · 6.35 Impact Factor
  • 07/2011;
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    ABSTRACT: We study the Kennicutt-Schmidt star formation law and efficiency in the gaseous disk of the isolated galaxy CIG 96 (NGC 864), with special emphasis on its unusually large atomic gas (H I) disk (r H mathsci/r 25 = 3.5, r 25 = 185). We present deep Galaxy Evolution Explorer near- and far-UV observations, used as a recent star formation tracer, and we compare them with new, high-resolution (16''or 1.6 kpc) Very Large Array H I observations. The UV and H I maps show good spatial correlation outside the inner 1', where the H I phase dominates over H2. Star-forming regions in the extended gaseous disk are mainly located along the enhanced H I emission within two (relatively) symmetric, giant gaseous spiral arm-like features, which emulate an H I pseudo-ring at r 3'. Inside this structure, two smaller gaseous spiral arms extend from the northeast and southwest of the optical disk and connect to the previously mentioned H I pseudo-ring. Interestingly, we find that the (atomic) Kennicutt-Schmidt power-law index systematically decreases with radius, from N 3.0 ± 0.3 in the inner disk (08-17) to N = 1.6 ± 0.5 in the outskirts of the gaseous disk (33-42). Although the star formation efficiency (SFE), the star formation rate per unit of gas, decreases with radius where the H I component dominates as is common in galaxies, we find that there is a break of the correlation at r = 1.5r 25. At radii 1.5r 25 < r < 3.5r 25, mostly within the H I pseudo-ring structure, regions exist whose SFE remains nearly constant, SFE 10–11 yr–1. We discuss possible mechanisms that might be triggering the star formation in the outskirts of this galaxy, and we suggest that the constant SFE for such large radii (r > 2r 25) and at such low surface densities might be a common characteristic in extended UV disk galaxies.
    The Astrophysical Journal 06/2011; 736(1):20. · 6.73 Impact Factor
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    ABSTRACT: (Abridged) We analyze the evolution of 42 spiral galaxies in the Spitzer Infrared Nearby Galaxies Survey, using extinction-corrected UV, optical and near-infrared radial profiles to probe the emission of stars of different ages as a function of radius. We fit these profiles with models that describe the chemical and spectro-photometric evolution of spiral disks within a self-consistent framework. These backward models succesfully reproduce the multi-wavelength profiles of our galaxies, except the UV profiles of some early-type disks. From the model fitting we infer the maximum circular velocity of the rotation curve (Vc) and the dimensionless spin parameter (lambda). The values of Vc are in good agreement with the velocities measured in HI rotation curves. While our sample is not volume-limited, the resulting distribution of spins is close to the lognormal function obtained in cosmological N-body simulations, peaking at ~0.03 regardless of the total halo mass. We do not find any evident trend between spin and Hubble type, besides an increase in the scatter for the latest types. According to the model, galaxies evolve along a roughly constant mass-size relation, increasing their scale-lengths as they become more massive. The radial scale-length of most disks in our sample seems to have increased at a rate of 0.05-0.06 kpc/Gyr, being now 20-25% larger than at z=1.
    The Astrophysical Journal 02/2011; 731(1). · 6.73 Impact Factor

Publication Stats

316 Citations
102.74 Total Impact Points

Institutions

  • 2014
    • European Southern Observatory
      Arching, Bavaria, Germany
  • 2013
    • Universidad de La Laguna
      • Department of Astrophysics
      San Cristóbal de La Laguna, Canary Islands, Spain
  • 2011–2013
    • National Radio Astronomy Observatory
      Charlottesville, Virginia, United States
  • 2007–2011
    • Universidad Complutense de Madrid
      • • Departamento de Física de la Tierra, Astronomía y Astrofísica II (Astrofísica y Ciencias de la Atmósfera)
      • • Department of Atomic, Molecular and Nuclear Physics
      Madrid, Madrid, Spain