DSpace Angular :: Browsing by Author "Quintana, H."

Browsing by Author "Quintana, H."

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Diffuse intracluster light at intermediate redshifts: intracluster light observations in an X-ray cluster at z=0.29
(2011) Toledo, I.; Melnick, J.; Selman, F.; Quintana, H.; Giraud, E.; Zelaya, P.
The diffuse intracluster light (ICL) contains a significant fraction of the total stellar mass in clusters of galaxies, and contributes in roughly equal proportion as the hot intracluster medium to the total baryon content of clusters. Because of the potential importance of understanding the origin of the ICL in the context of the formation and evolution of structure in the Universe, the field has recently undergone a revival both in the quality and quantity of observational and theoretical investigations. Because of cosmological dimming, the observational work has mostly concentrated on low-redshift clusters, but clearly observations at higher redshifts can provide interesting clues about the evolution of the diffuse component. In this paper we present the first results of a programme to characterize the ICL of intermediate-redshift clusters. We find that at z similar to 0.3, the X-ray cluster RXJ0054.0-2823 already has a significant ICL and that the fraction of the total light in the ICL and the brightest cluster galaxy (BCG) is comparable to that of similar clusters at lower redshift. We also find that the kinematics of the ICL is consistent with it being the remnant of tidally destroyed galaxies streaming in the central regions of the cluster, which has three central giant elliptical galaxies acting as an efficient 'galaxy grinding machine'. Our cluster has a bi-modal radial velocity distribution and thus two possible values for the velocity dispersion. We find that the cluster fits well in the correlation between BCG+ICL fraction and cluster mass for a range of velocity dispersions, leading us to question the validity of a relevant correlation between these two quantities.
Discovery of a massive X-ray luminous galaxy cluster at z=1.579
(2011) Santos, J. S.; Fassbender, R.; Nastasi, A.; Boehringer, H.; Rosati, P.; Suhada, R.; Pierini, D.; Nonino, M.; Muehlegger, M.; Quintana, H.; Schwope, A. D.; Lamer, G.; de Hoon, A.; Strazzullo, V.
We report on the discovery of a very distant galaxy cluster serendipitously detected in the archive of the XMM-Newton mission, within the scope of the XMM-Newton Distant Cluster Project (XDCP). XMMUJ0044.0-2033 was detected at a high significance level (5 sigma) as a compact, but significantly extended source in the X-ray data, with a soft-band flux f(r < 40 '') = (1.5 +/- 0.3) x 10(-14) erg s(-1) cm(2). Optical/NIR follow-up observations confirmed the presence of an overdensity of red galaxies matching the X-ray emission. The cluster was spectroscopically confirmed to be at z = 1.579 using ground-based VLT/FORS2 spectroscopy. The analysis of the I-H colour-magnitude diagram shows a sequence of red galaxies with a colour range [3.7 < I-H < 4.6] within 1' from the cluster X-ray emission peak. However, the three spectroscopic members (all with complex morphology) have significantly bluer colours relative to the observed red-sequence. In addition, two of the three cluster members have [OII] emission, indicative of on-going star formation. Using the spectroscopic redshift we estimated the X-ray bolometric luminosity, L-bol,L-40 '' similar to 5.8 x 10(44) erg s(-1), implying a massive galaxy cluster. This places XMMU J0044.0-2033 at the forefront of massive distant clusters, closing the gap between lower redshift systems and recently discovered proto-and low-mass clusters at z > 1.6.
Distant galaxy clusters in a deep XMM-Newton field within the CFTHLS D4
(2013) de Hoon, A.; Lamer, G.; Schwope, A.; Muehlegger, M.; Fassbender, R.; Boehringer, H.; Lerchster, M.; Nastasi, A.; Suhada, R.; Verdugo, M.; Dietrich, J. P.; Brimioulle, F.; Rosati, P.; Pierini, D.; Santos, J. S.; Quintana, H.; Rabitz, A.; Takey, A.
Aims. The XMM-Newton distant cluster project (XDCP) aims at the identification of a well defined sample of X-ray selected clusters of galaxies at redshifts z >= 0.8. As part of this project, we analyse the deep XMM-Newton exposure covering one of the CFHTLS deep fields to quantify the cluster content. We validate the optical follow-up strategy as well as the X-ray selection function.
Exploring the galaxy cluster-group transition regime at high redshifts Physical properties of two newly detected z > 1 systems
(2011) Suhada, R.; Fassbender, R.; Nastasi, A.; Boehringer, H.; de Hoon, A.; Pierini, D.; Santos, J. S.; Rosati, P.; Muehlegger, M.; Quintana, H.; Schwope, A. D.; Lamer, G.; Kohnert, J.; Pratt, G. W.
Context. Multi-wavelength surveys for clusters of galaxies are opening a window on the elusive high-redshift (z > 1) cluster population. Well controlled statistical samples of distant clusters will enable us to answer questions about their cosmological context, early assembly phases and the thermodynamical evolution of the intracluster medium.
First simultaneous optical/near-infrared imaging of an X-ray selected, high-redshift cluster of galaxies with GROND The galaxy population of XMMU J0338.7+0030 at z=1.1
(2012) Pierini, D.; Suhada, R.; Fassbender, R.; Nastasi, A.; Boehringer, H.; Salvato, M.; Pratt, G. W.; Lerchster, M.; Rosati, P.; Santos, J. S.; de Hoon, A.; Kohnert, J.; Lamer, G.; Mohr, J. J.; Muehlegger, M.; Quintana, H.; Schwope, A.; Biffi, V.; Chon, G.; Giodini, S.; Koppenhoefer, J.; Verdugo, M.; Ziparo, F.; Afonso, P. M. J.; Clemens, C.; Greiner, J.; Kruehler, T.; Yoldas, A. Kuepcue; Olivares E, F.; Rossi, A.; Yoldas, A.
Context. The XMM-Newton Distant Cluster Project is a serendipitous survey for clusters of galaxies at redshifts z >= 0.8 based on deep archival XMM-Newton observations. X-ray sources identified as extended are screened against existing optical all-sky surveys for galaxies, in case of candidate high-z clusters followed up with imaging at 4 m-class telescopes and, ultimately, multi-object spectroscopy at 8 m-class telescopes. Low-significance candidate high-z clusters are followed up with the seven-channel imager GROND (Gamma-Ray Burst Optical and Near-Infrared Detector) that is mounted at a 2 m-class telescope. Its unique capability of simultaneous imaging in the g', r', i', z', J, H, Ks bands enables the use of the photometric redshift technique.
Galaxy Evolution in a Pilot Survey up to z=1 and CDM Halos
(2011) Giraud, E.; Melnick, J.; Gu, Q. -S.; Quintana, H.; Selman, F.; Toledo, I.; Zelaya, P.
We study spectral evolution of galaxies in a magnitude limited sample of 550 galaxies from z = 1 down to z = 0.3 on a pencil beam of approximate to 10' x 10'. We concentrate on the large apparent cosmological structures along the line of sight, and we bin our individual galaxy spectra to obtain representative high S/N spectra based upon these structures. We divide the resulting average spectra in three groups to facilitate the analysis: galaxies with pure absorption line spectra, galaxies with emission lines and blue continua, and galaxies with emission lines and red continua. We revisit the question of downsizing in emission-line galaxies between z = 0.9 and z = 0.45 in our pencil-beam and find the following results: strong star formation in emission line galaxies, aging in emission line galaxies, and aging in absorption systems, are shifting from bright to faint systems as cosmological time increases. Each redshift bin is repopulated in new starbursts. Therefore at redshifts z <= 1 galaxy formation is downsizing both in luminosity and number density. Our observations indicate that at z <= 1 star formation and hierarchical structure formation of CDM halos are not in phase.
Kinematic analysis of a sample of X-ray luminous distant galaxy clusters The L_x-σ_v relation in the z > 0.6 universe
(2014) Nastasi, A.; Boehringer, H.; Fassbender, R.; De Hoon, A.; Lamer, G.; Mohr, J. J.; Padilla, N.; Pratt, G. W.; Quintana, H.; Rosati, P.; Santos, J. S.; Schwope, A. D.; Suhada, R.; Verdugo, M.
Aims. Observations and cosmological simulations show galaxy clusters as a family of nearly self-similar objects with properties that can be described by scaling relations as a function of mass and time. Here we study the scaling relations between the galaxy velocity dispersion (sigma(v)) and X-ray quantities, such as X-ray bolometric luminosity (L-X,500(Bol)) and temperature (T-X) in galaxy clusters at high redshifts (0.64 <= z <= 1.46). We also compare our results with the analogous study of the local HIFLUGCS sample.
Photometry of the Central Regions in a Complete Sample of High Bautz-Morgan-Type Abell Clusters. I. Observations and Data Calibration
(2000) Quintana, H.; Infante, L.; Fouque, P.; Carrasco, E.R.; Cuevas, H.; Hertling, G.; Nuñez, I.
We present CCD photometry of 209 southern Abell clusters selected according to Bautz-Morgan type I, I-II, and II. We have performed total photometry in the GUM r bandpass, classified stars and galaxies, and obtained structural parameters for the images. To estimate the photometric and structural errors on the CCD images and the completeness limits of our photometry, we performed realistic simulations of stars and galaxies and ran our classification algorithms. Here, we present central galaxy counts and metric photometry of the brightest cluster,:members, for which we give accurate positions, and compare this photometry with values in the literature. A linear magnitude-redshift relation has been derived from the tenth-ranked galaxy in each cluster. Photometric redshifts have been estimated for 57 clusters. We provide either spectroscopic or photometric redshifts for all the clusters in our sample. Further analysis of these data will be presented in further publications.
Scaling relations of the colour-detected cluster RzCS 052 at z=1.016 and some other high-redshift clusters
(2008) Andreon, S.; De Propris, R.; Puddu, E.; Giordano, L.; Quintana, H.
We report on the discovery of the z = 1.016 cluster RzCS 052 using a modified red-sequence method, follow up spectroscopy and X-ray imaging. This cluster has a velocity dispersion of 710 +/- 150 km s(-1), a virial mass of 4.0 x 10(14) M-circle dot (based on 21 spectroscopically confirmed members) and an X-ray luminosity of (0.68 +/- 0.47) x 10(44) erg s(-1) in the [1-4] keV band. This optically selected cluster appears to be of richness class 3 and to follow the known L-X-sigma(v) relation for high-redshift X-ray selected clusters. Using these data, we find that the halo occupation number for this cluster is only marginally consistent with what was expected assuming a self-similar evolution of cluster scaling relations, suggesting perhaps a break of them at z similar to 1. We also rule out a strong galaxy merging activity between z = 1 and today. Finally, we present a Bayesian approach to measuring cluster velocity dispersions and X-ray luminosities in the presence of a background: we critically reanalyse recent claims for X-ray underluminous clusters using these techniques and find that the clusters can be accommodated within the existing L-X-sigma(v) relation.
Structure and dynamics of the Shapley Supercluster -: Velocity catalogue, general morphology and mass
(2006) Proust, D.; Quintana, H.; Carrasco, E.R.; Reisenegger, A.; Slezak, E.; Muriel, H.; Dünner, R.; Sodre, L.; Drinkwater, M.J.; Parker, Q.A.; Ragone, C.J.
We present results of our wide-field redshift survey of galaxies in a 285 square degree region of the Shapley Supercluster (SSC), based on a set of 10 529 velocity measurements (including 1201 new ones) on 8632 galaxies obtained from various telescopes and from the literature. Our data reveal that the main plane of the SSC (v approximate to 14 500 km s(-1)) extends further than previous estimates, filling the whole extent of our survey region of 12 degrees by 30 degrees on the sky (30 x 75 h(-1) Mpc). There is also a connecting structure associated with the slightly nearer Abell 3571 cluster complex (v approximate to 12 000 km s(-1)). These galaxies seem to link two previously identified sheets of galaxies and establish a connection with a third one at v = 15 000 km s(-1) near RA = 13(h). They also tend to fill the gap of galaxies between the foreground Hydra-Centaurus region and the more distant SSC. In the velocity range of the Shapley Supercluster (9000 km s(-1) < cz < 18 000 km s(-1)), we found redshift-space overdensities with b(j) < 17.5 of similar or equal to 5.4 over the 225 square degree central region and similar or equal to 3.8 in a 192 square degree region excluding rich clusters. Over the large region of our survey, we find that the intercluster galaxies make up 48 per cent of the observed galaxies in the SSC region and, accounting for the different completeness, may contribute nearly twice as much mass as the cluster galaxies. In this paper, we discuss the completeness of the velocity catalogue, the morphology of the supercluster, the global overdensity, and some properties of the individual galaxy clusters in the Supercluster.
The Atacama Cosmology Telescope (ACT): Beam Profiles and First SZ Cluster Maps
(2010) Hincks, A. D.; Acquaviva, V.; Ade, P. A. R.; Aguirre, P.; Amiri, M.; Appel, J. W.; Barrientos, L. F.; Battistelli, E. S.; Bond, J. R.; Brown, B.; Burger, B.; Chervenak, J.; Das, S.; Devlin, M. J.; Dicker, S. R.; Doriese, W. B.; Dunkley, J.; Dünner, R.; Essinger-Hileman, T.; Fisher, R. P.; Fowler, J. W.; Hajian, A.; Halpern, M.; Hasselfield, M.; Hernández-Monteagudo, C.; Hilton, G. C.; Hilton, M.; Hlozek, R.; Huffenberger, K. M.; Hughes, D. H.; Hughes, J. P.; Infante, L.; Irwin, K. D.; Jimenez, R.; Juin, J. B.; Kaul, M.; Klein, J.; Kosowsky, A.; Lau, J. M.; Limon, M.; Lin, Y. -T.; Lupton, R. H.; Marriage, T. A.; Marsden, D.; Martocci, K.; Mauskopf, P.; Menanteau, F.; Moodley, K.; Moseley, H.; Netterfield, C. B.; Niemack, M. D.; Nolta, M. R.; Page, L. A.; Parker, L.; Partridge, B.; Quintana, H.; Reid, B.; Sehgal, N.; Sievers, J.; Spergel, D. N.; Staggs, S. T.; Stryzak, O.; Swetz, D. S.; Switzer, E. R.; Thornton, R.; Trac, H.; Tucker, C.; Verde, L.; Warne, R.; Wilson, G.; Wollack, E.; Zhao, Y.
The Atacama Cosmology Telescope (ACT) is currently observing the cosmic microwave background with arcminute resolution at 148 GHz, 218 GHz, and 277 GHz. In this paper, we present ACT's first results. Data have been analyzed using a maximum-likelihood map-making method which uses B-splines to model and remove the atmospheric signal. It has been used to make high-precision beam maps from which we determine the experiment's window functions. This beam information directly impacts all subsequent analyses of the data. We also used the method to map a sample of galaxy clusters via the Sunyaev-Zel'dovich (SZ) effect and show five clusters previously detected with X-ray or SZ observations. We provide integrated Compton-y measurements for each cluster. Of particular interest is our detection of the z = 0.44 component of A3128 and our current non-detection of the low-redshift part, providing strong evidence that the further cluster is more massive as suggested by X-ray measurements. This is a compelling example of the redshift-independent mass selection of the SZ effect.
The Atacama Cosmology Telescope : cosmological parameters from three seasons of data
(2013) Sievers, J.; Hlozek, R. A.; Nolta, M. R.; Acquaviva, V.; Adisson, G. E.; Ade, P.A.R.; Aguirre, Paula; Amiri, M.; Appel, J. W.; Barrientos, Luis Felipe; Gallardo, P.; Infante Lira, Leopoldo; Quintana, H.; Rojas, F. et al.
THE ATACAMA COSMOLOGY TELESCOPE: A MEASUREMENT OF THE 600 < ℓ < 8000 COSMIC MICROWAVE BACKGROUND POWER SPECTRUM AT 148 GHz
(2010) Fowler, J. W.; Acquaviva, V.; Ade, P. A. R.; Aguirre, P.; Amiri, M.; Appel, J. W.; Barrientos, L. F.; Battistelli, E. S.; Bond, J. R.; Brown, B.; Burger, B.; Chervenak, J.; Das, S.; Devlin, M. J.; Dicker, S. R.; Doriese, W. B.; Dunkley, J.; Dünner, R.; Essinger-Hileman, T.; Fisher, R. P.; Hajian, A.; Halpern, M.; Hasselfield, M.; Hernández-Monteagudo, C.; Hilton, G. C.; Hilton, M.; Hincks, A. D.; Hlozek, R.; Huffenberger, K. M.; Hughes, D. H.; Hughes, J. P.; Infante, L.; Irwin, K. D.; Jimenez, R.; Juin, J. B.; Kaul, M.; Klein, J.; Kosowsky, A.; Lau, J. M.; Limon, M.; Lin, Y. -T.; Lupton, R. H.; Marriage, T. A.; Marsden, D.; Martocci, K.; Mauskopf, P.; Menanteau, F.; Moodley, K.; Moseley, H.; Netterfield, C. B.; Niemack, M. D.; Nolta, M. R.; Page, L. A.; Parker, L.; Partridge, B.; Quintana, H.; Reid, B.; Sehgal, N.; Sievers, J.; Spergel, D. N.; Staggs, S. T.; Swetz, D. S.; Switzer, E. R.; Thornton, R.; Trac, H.; Tucker, C.; Verde, L.; Warne, R.; Wilson, G.; Wollack, E.; Zhao, Y.
We present a measurement of the angular power spectrum of the cosmic microwave background (CMB) radiation observed at 148 GHz. The measurement uses maps with 1'.4 angular resolution made with data from the Atacama Cosmology Telescope (ACT). The observations cover 228 deg(2) of the southern sky, in a 4 degrees.2 wide strip centered on declination 53 degrees south. The CMB at arcminute angular scales is particularly sensitive to the Silk damping scale, to the Sunyaev-Zel'dovich (SZ) effect from galaxy clusters, and to emission by radio sources and dusty galaxies. After masking the 108 brightest point sources in our maps, we estimate the power spectrum between 600 < l < 8000 using the adaptive multi-taper method to minimize spectral leakage and maximize use of the full data set. Our absolute calibration is based on observations of Uranus. To verify the calibration and test the fidelity of our map at large angular scales, we cross-correlate the ACT map to the WMAP map and recover the WMAP power spectrum from 250 < l < 1150. The power beyond the Silk damping tail of the CMB (l similar to 5000) is consistent with models of the emission from point sources. We quantify the contribution of SZ clusters to the power spectrum by fitting to a model normalized to sigma(8) = 0.8. We constrain the model's amplitude A(SZ) < 1.63 (95% CL). If interpreted as a measurement of sigma(8), this implies sigma(SZ)(8) < 0.86 (95% CL) given our SZ model. A fit of ACT and WMAP five-year data jointly to a six-parameter Lambda CDM model plus point sources and the SZ effect is consistent with these results.
The shapley supercluster. III. Collapse dynamics and mass of the central concentration
(2000) Reisenegger, A.; Quintana, H.; Carrasco, E.R.; Maze, J.
We present the first application of a spherical collapse model to a supercluster of galaxies. Positions and redshifts of similar to 3000 galaxies in the Shapley supercluster (SSC) are used to define velocity caustics that limit the gravitationally collapsing structure in its central part. This is found to extend at least to 8 h(-1) Mpc of the central cluster, A3558, enclosing 11 ACO clusters. Infall velocities reach similar to 2000 km s(-1). Dynamical models of the collapsing region are used to estimate its mass profile. An upper bound on the mass, based on a pure spherical infall model, gives M(<8 h(-1) Mpc) less than or similar to 1.3 x 10(16) h(-1) M. for an Einstein-de Sitter (critical) universe and M(<8 h(-1) Mpc) less than or similar to 8.5 x 10(15) h(-1) M. for an empty universe. The Diaferio & Geller model, based on estimating the escape velocity, gives a significantly lower value, M(<8 h(-1) Mpc) approximate to 2.1 x 10(15) h(-1) M., very similar to the mass Geller et al. found around the Coma cluster by the same method and comparable to or slightly lower than the dynamical mass in the vriialized regions of clusters enclosed in the same region of the SSC. In both models, the overdensity in this region is substantial, but it is far from the value required to account for the peculiar motion of the Local Group with respect to the cosmic microwave background.

Browsing by Author "Quintana, H."

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