Vicent J. Martı́nez

Universitat de València

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A. Fernández-Soto

Universitat de València

E. Saar

Estonian Academy of Sciences

M. Moles

Centro de Estudios de Física del Cosmos de Aragón

N. Benı́tez

Instituto de Astrofísica de Andalucía

I. Márquez

Instituto de Astrofísica de Andalucía

D. Cristòbal-Hornillos

Centro de Estudios de Física del Cosmos de Aragón

R. M. González Delgado

Instituto de Astrofísica de Andalucía

E. J. Alfaro

Instituto de Astrofísica de Andalucía

Tom Broadhurst

University of the Basque Country

J. Cepa

Universidad de La Laguna

Cooperative Institutions

Centro de Estudios de Física del Cosmos de Aragón

Consejo Superior de Investigaciones Científicas

Instituto de Astrofísica de Andalucía

Instituto de Astrofísica de Canarias

Centre National de la Recherche Scientifique

Valongo Observatory

Universidad de La Laguna

Universidad Complutense de Madrid

Universidade de São Paulo

National Observatory

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Point field models for the galaxy point pattern. Modelling the singularity of the two-point correlation function

arXiv (Cornell University) (2002)

Martin Snethlage Vicent J. Martı́nez Dietrich Stoyan E. Saar

There is empirical evidence that the two-point correlation function of the galaxy distribution follows, for small scales, reasonably well a power-law expression $\xi(r)\propto r^{-\gamma}$ with $\gamma$ between 1.5 and 1.9. Nevertheless, most of the point field models suggested in the literature do not have this property. This paper presents a new class of models, which is produced by modifying point fields commonly used in cosmology to mimic the galaxy distribution, but where $\gamma=2$ is too large. The points are independently and randomly shifted, leading to the desired reduction of the value of $\gamma$.

Empirical distribution function

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Lyman Break and ultraviolet-selected galaxies at z ∼ 1 – II. PACS 100 μm/160 μm FIR detections★

Monthly Notices of the Royal Astronomical Society (2013)

I. Oteo G. Magdis Á. Bongiovanni A. M. Pérez García J. Cepa

In this work, we report the Photodetector Array Camera and Spectrometer (PACS) 100 μm/160 μm detections of a sample of 42 GALEX-selected and far-infrared (FIR)-detected Lyman break galaxies (LBGs) at z ∼ 1 located in the Cosmic Evolution Survey (COSMOS) field and analyse their ultraviolet (UV) to FIR properties. The detection of these LBGs in the FIR indicates that they have a dust content high enough so that its emission can be directly detected. According to a spectral energy distribution (SED) fitting with stellar population templates to their UV-to-near-IR observed photometry, PACS-detected LBGs tend to be bigger (Reff ∼ 4.1 kpc), more massive [log (M*/M⊙) ∼ 10.7], dustier [Es(B − V) ∼ 0.40], redder in the UV continuum (β ∼ −0.60) and UV-brighter [log (LUV/L⊙) ∼ 10.1] than PACS-undetected LBGs. PACS-detected LBGs at z ∼ 1 are mostly disc-like galaxies and are located over the green valley and red sequence of the colour–magnitude diagram of galaxies at their redshift. By using their UV and IR emission, we find that PACS-detected LBGs tend to be less dusty and have slightly higher total star formation rates (SFRs) than other PACS-detected UV-selected galaxies within the same redshift range. As a consequence of the selection effect due to the depth of the FIR observations employed, all our PACS-detected LBGs have total IR luminosities, LIR, higher than 1011 L⊙ and thus are luminous IR galaxies. However, none of the PACS-detected LBGs are in the ultra-luminous IR galaxy (ULIRG) regime, LIR ≥ 1012 L⊙, where the FIR observations are complete. The finding of ULIRGs-LBGs at higher redshifts (z ∼ 3) suggests an evolution of the FIR emission of LBGs with cosmic time. In an IRX–β diagram, PACS-detected LBGs at z ∼ 1 tend to be located around the relation for local starburst similarly to other UV-selected PACS-detected galaxies at the same redshift. Consequently, the dust-correction factors obtained with their UV continuum slope allow us to determine their total SFR, unlike at higher redshifts. However, the dust attenuation derived from UV to NIR SED fitting overestimates the total SFR for most of our PACS-detected LBGs in an age-dependent way: the overestimation factor is higher in younger galaxies. This is likely due to the typical degeneracy between dust attenuation and age in the SED fitting with synthetic templates and highlights the importance of the FIR measurements in the analysis of star-forming galaxies at intermediate redshifts.

Spectral energy distribution

Ultraviolet

10.1093/mnras/stt1244

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The ALHAMBRA survey: 2D analysis of the stellar populations in massive early-type galaxies atz< 0.3

Astronomy and Astrophysics (2017)

I. San Roman A. J. Cenarro L. A. Díaz-García C. López-Sanjuán J. Varela

We present a technique that permits the analysis of stellar population gradients in a relatively low-cost way compared to integral field unit (IFU) surveys. We developed a technique to analyze unresolved stellar populations of spatially resolved galaxies based on photometric multi-filter surveys. This technique allows the analysis of vastly larger samples and out to larger galactic radii. We derived spatially resolved stellar population properties and radial gradients by applying a centroidal Voronoi tessellation and performing a multicolor photometry spectral energy distribution fitting. This technique has been successfully applied to a sample of 29 massive ( M ⋆ > 10 10.5 M ⊙ ) early-type galaxies at z < 0.3 from the ALHAMBRA survey. We produced detailed 2D maps of stellar population properties (age, metallicity, and extinction), which allow us to identify galactic features. Radial structures were studied, and luminosity-weighted and mass-weighted gradients were derived out to 2–3.5 R eff . We find that the spatially resolved stellar population mass, age, and metallicity are well represented by their integrated values. We find the gradients of early-type galaxies to be on average flat in age (∇log Age L = 0.02 ± 0.06 dex/ R eff ) and negative in metallicity (∇[Fe/H] L = −0.09 ± 0.06 dex/ R eff ). Overall,the extinction gradients are flat (∇ A v = −0.03 ± 0.09 mag/ R eff ) with a wide spread. These results are in agreement with previous studies that used standard long-slit spectroscopy, and with the most recent IFU studies. According to recent simulations, these results are consistent with a scenario where early-type galaxies were formed through major mergers and where their final gradients are driven by the older ages and higher metallicity of the accreted systems. We demonstrate the scientific potential of multi-filter photometry to explore the spatially resolved stellar populations of local galaxies and confirm previous spectroscopic trends from a complementary technique.

Stellar population

Extinction (optical mineralogy)

Stellar mass

10.1051/0004-6361/201630313

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Transparències galàctiques en la foscor de la nit

Vicent J. Martı́nez

10.2436/mètode.v0i0.46408

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Recent Advances in Large-scale Structure Statistics

Springer eBooks (1997)

Vicent J. Martı́nez

10.1007/978-1-4612-1968-2_9

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THE ALHAMBRA PHOTOMETRIC SYSTEM

The Astronomical Journal (2010)

T. Aparicio Villegas E. J. Alfaro J. Cabrera-Caño M. Moles N. Benı́tez

This paper presents the characterization of the optical range of the ALHAMBRA photometric system, a 20 contiguous, equal-width, medium-band CCD system with wavelength coverage from 3500A to 9700A. The photometric description of the system is done by presenting the full response curve as a product of the filters, CCD and atmospheric transmission curves, and using some first and second order moments of this response function. We also introduce the set of standard stars that defines the system, formed by 31 classic spectrophotometric standard stars which have been used in the calibration of other known photometric systems, and 288 stars, flux calibrated homogeneously, from the Next Generation Spectral Library (NGSL). Based on the NGSL, we determine the transformation equations between Sloan Digital Sky Survey (SDSS) ugriz photometry and the ALHAMBRA photometric system, in order to establish some relations between both systems. Finally we develop and discuss a strategy to calculate the photometric zero points of the different pointings in the ALHAMBRA project.

Photometric system

10.1088/0004-6256/139/3/1242

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Citations (42)

SDSS DR7 superclusters

Astronomy and Astrophysics (2011)

M. Einasto L. J. Liivamägi E. Tago E. Saar Elmo Tempel

We study the morphology of a set of superclusters drawn from the SDSS DR7. We calculate the luminosity density field to determine superclusters from a flux- limited sample of galaxies from SDSS DR7, and select superclusters with 300 and more galaxies for our study. The morphology of superclusters is described with the fourth Minkowski functional V3, the morphological signature (the curve in the shapefinder's K1-K2 plane) and the shape parameter (the ratio of the shapefinders K1/K2). We investigate the supercluster sample using multidimensional normal mixture modelling, and use Abell clusters to identify our superclusters with known superclusters and to study the large-scale distribution of superclusters. The superclusters in our sample form three chains of superclusters; one of them is the Sloan Great Wall. Most superclusters have filament-like overall shapes. Superclusters can be divided into two sets; more elongated superclusters are more luminous, richer, have larger diameters, and a more complex fine structure than less elongated superclusters. The fine structure of superclusters can be divided into four main morphological types: spiders, multispiders, filaments, and multibranching filaments. We present the 2D and 3D distribution of galaxies and rich groups, the fourth Minkowski functional, and the morphological signature for all superclusters. Widely different morphologies of superclusters show that their evolution has been dissimilar. A study of a larger sample of superclusters from observations and simulations is needed to understand the morphological variety of superclusters and the possible connection between the morphology of superclusters and their large-scale environment.

Supercluster (genetic)

10.1051/0004-6361/201116564

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Citations (46)

Desvelant l'univers: Veïns?

Mètode: Revista de difusió de la investigació (2016)

Vicent J. Martı́nez

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Imaginació i ciència: Un binomi inseparable: entitats indetectables però essencials per als astrònoms del passat i del present

Mètode: Revista de difusió de la investigació de la Universitat de Valencia (2012)

Vicent J. Martı́nez Virginia Trimble

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Satellites of Isolated Elliptical Galaxies

arXiv (Cornell University) (2003)

Rodney Smith Vicent J. Martı́nez

Using well-defined selection criteria applied to the LEDA galaxy catalogue we have derived a sample of elliptical galaxies that can be classified as isolated. From this we have investigated the neighbourhood of these galaxies to determine the frequency and radial distribution of faint galaxies around them and hence derive an estimate of their surrounding satellite population. The results are compared and contrasted to the satellite population around isolated spiral galaxies.

Satellite galaxy

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