Person: Castillo Morales, María África
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First Name
María África
Last Name
Castillo Morales
Affiliation
Universidad Complutense de Madrid
Faculty / Institute
Ciencias Físicas
Department
Física de la Tierra y Astrofísica
Area
Astronomía y Astrofísica
Identifiers
10 results
Search Results
Now showing 1 - 10 of 10
Item XMM observation of the dynamically young galaxy cluster CL 0939+4713(Astronomy and astrophysics, 2003) De Filippis, E.; Schindler, S.; Castillo Morales, María ÁfricaWe present an XMM observation of the distant galaxy cluster CL 0939+4713. The X-ray image shows pronounced substructure, with two main subclusters which have even some internal structure. This is an indication that the cluster is a dynamically young system. This conclusion is supported by the temperature distribution: a hot region is found between the two main subclusters indicating that they are at the beginning of a major merger, and that they will probably collide in a few hundreds of Myr. The intra-cluster gas of CL 0939+4713 shows inhomogeneities in the metal distribution, with the optically richer subcluster having a higher metallicity.Item Truncated stellar disks in the near infrared I. Observations(Astronomy and astrophysics, 2006) Florido, E.; Battaner, E.; Guijarro, A.; Garzón, F.; Castillo Morales, María ÁfricaWe present NIR surface photometry of 11 edge-on galaxies obtained in the course of a long term project aimed at analysing the occurrence and type of the truncation of the outer disks. Observations were carried out at the 1.5 m CST (Carlos Sanchez Telescope) in Tenerife (Spain) using the CAIN infrared camera. 7 galaxies exhibit clear truncation on their disk profiles and 4 galaxies were observed to be clearly untruncated within observational limits. We describe the truncations as real, smooth and complete (as suggested by extrapolation and in the sense that the measured truncation curve goes into the noise at a truncation radius R(tr)), following a decline proportional to (R(tr)-R)(-n) (where R is the radius). Despite its deep photometric reach, the data presented do not permit a detailed exploration of the region where optical data show a second slope. Special care was taken concerning the surface brightness deprojection of edge-on galaxies, which was carried out by two methods, one comprising the inversion of Abel's integral equation and the other following a numerical method. These methods gave nearly identical results. NIR observations of truncations could differ from observations in the optical, since the two domains trace different stellar populations.Item Truncated stellar discs in the near infrared II. Statistical properties and interpretation(Astronomy and astrophysics, 2006) Florido, E.; Battaner, E.; Guijarro, A.; Garzón, F.; Castillo Morales, María ÁfricaThe results obtained in Paper I are used to study possible relationships between the truncation radius of stellar discs in the NIR and structural parameters of the galaxies. The NIR truncation radius is larger for brighter galaxies, being proportional to V(m)(c) with c approximate to 3/2, and with V(m) being the asymptotic rotation velocity at large radii (when the rotation curve becomes flat), and is lower for higher wavelengths. When it is normalized to the scalelength, the truncation is an increasing function of the central surface brightness and is lower for late type galaxies, although these correlations are weaker. These relations are in agreement with the scenario of magnetically driven truncations.Item Non-circular motion evidence in the circumnuclear region of M100 (NGC 4321)(Monthly notices of the Royal Astronomical Society, 2007) Castillo Morales, María África; Jiménez Vicente, J.; Mediavilla, E.; Battaner, E.We analyse new integral-field spectroscopy of the inner region (central 2.5 kpc) of the spiral galaxy NGC 4321 to study the peculiar kinematics of this region. Fourier analysis of the velocity residuals obtained by subtracting an axisymmetric rotation model from the H alpha velocity field indicates that the distortions are global features generated by an m = 2 perturbation of the gravitational potential which can be explained by the nuclear bar. This bar has been previously observed in the near-infrared but not in the optical continuum dominated by star formation. We detect the optical counterpart of this bar in the 2D distribution of the old stellar population (inferred from the equivalent width map of the stellar absorption lines). We apply the Tremaine-Weinberg method to the stellar velocity field to calculate the pattern speed of the inner bar, obtaining a value of Omega(b) = 160 +/- 70 km s(-1) kpc(-1). This value is considerably larger than the one obtained when a simple bar model is considered. However, the uncertainties in the pattern speed determination prevent us from giving support to alternative scenarios.Item Asymmetrical structure of ionization and kinematics in the Seyfert galaxy NGC 5033(Astronomy and astrophysics, 2005) Mediavilla, E.; Guijarro, A.; Castillo Morales, María África; Jiménez Vicente, J.; Florido, E.; Arribas, S.; García Lorenzo, B.; Battaner, E.We present integral field spectroscopy of NGC 5033, a low luminosity Seyfert galaxy. The observations were made with INTEGRAL, a fiber based system operating at the WHT. The intensity map of the H emission line represents a spiral or ring-like pattern of HII regions. On the contrary, the [OIII] intensity map morphology is markedly anisotropic. The strong morphological differences imply that the [ OIII] emitters represent highly ionized gas illuminated by the central source. The [ OIII] map morphology is compatible with a biconical structure of ionization induced by strong extinction in the galaxy disc that also obscures half of the spheroidal stellar bulge. We identify the spectrum corresponding to the Seyfert 1 nucleus from the presence of H broad emission lines. This spectrum is located in a region where strong extinction is expected but exhibits the bluest spectral energy distribution. The Seyfert 1 nucleus seems to be off center with respect to the stellar rotation center. This result has been also found in other Seyfert galaxies and interpreted in terms of a past merger. The off centering could indicate the presence of nonsymmetric departures in the gravitational potential which could be fueling the active nucleus. The kinematics of the [ OIII] emitters show important deviations at a kpc scale with respect to the stellar velocity field and show features related to the asymmetrical morphology of the high ionization region.Item Discovery of depressions in the X-ray emission of the distant galaxy cluster RBS797 in a CHANDRA observation(Astronomy and astrophysics, 2001) Schindler, S.; Castillo Morales, María África; De Filippis, E.; Schwope, A.; Wambsganss, J.We present CHANDRA observations of the X-ray luminous, distant galaxy cluster RBS797 at z = 0.35. In the central region the X-ray emission shows two pronounced X-ray minima, which are located opposite to each other with respect to the cluster centre. These depressions suggest an interaction between the central radio galaxy and the intra-cluster medium, which would be the first detection in such a distant cluster. The minima are symmetric relative to the cluster centre and very deep compared to similar features found in a few other nearby clusters. A spectral and morphological analysis of the overall cluster emission shows that RBS797 is a hot cluster (T = 7.7(-1.0)(+1.2) keV) with a total mass of M-tot(r(500)) = 6.5(-1.2)(+1.6) x 10(14) M-..Item Distribution of baryonic and non-baryonic matter in clusters of galaxies(Tracing cosmic evolution with galaxy clusters, proceedings, 2002) Castillo Morales, María África; Schindler, S.We present the analysis of baryonic and non-baryonic matter distributions in a sample of eleven nearby clusters (0.03 < z < 0.09) with temperatures between 4.4 and 9.4 keV. These galaxy clusters have been studied in detail using X-ray data and global physical properties have been determined. Correlations between these quantities have been analysed and compared with the results for distant clusters. We found an interesting dependence between the relative gas extent (expressed as the ratio of gas mass fractions at r(500) and 0.5 x r(500)) and the total cluster mass. The extent of the gas relative to the extent of the dark matter tends to be larger in less massive clusters. This dependence might give us some hints about non-gravitational processes in clusters.Item Discovery of a galactic wind in the central region of M100(Monthly notices of the Royal Astronomical Society, 2007) Jiménez Vicente, J.; Castillo Morales, María África; Mediavilla, E; Battaner, E.We report the discovery of a galactic wind in the central region of the galaxy M100. This result is based on a careful 2D spectroscopic study performed on observations made with the fibre system INTEGRAL on the William Herschel Telescope. The primary evidence of the wind is the presence of blueshifted interstellar NaD absorption lines. The velocity field of the absorbers show a clear rotation pattern but which is globally blueshifted (similar to -115 km s(-1)) with respect to the systemic velocity of the galaxy. The emission lines also present a blueward component arising from the ionized gas phase of the galactic wind. The velocity field of the ionized gas wind component shows no evidence of rotation but exhibits a pattern that can be interpreted in terms of the projection of an outflowing cone or shell. The wind component has [N II]/H alpha ratios of about 1.8, typical of shock ionization. The ionized component of the wind can be identified with an expanding shell of shocked gas, and the neutral component with disc gas entrained in the wind at the interface of the expanding shell with the galactic interstellar medium. The galactic wind seems to be driven uniquely by the nuclear starburst. Our analysis indicates that a non-negligible fraction of the wind material might escape to the intergalactic medium (IGM). In this case, if the wind detected in M100 were representative of similar phenomena in other galaxies with low to moderate activity, the current estimates of metal and dust content of the IGM might be drastically underestimated.Item Distribution of dark and baryonic matter in clusters of galaxies(Astronomy and astrophysics, 2003) Castillo Morales, María África; Schindler, S.We present the analysis of baryonic and non-baryonic matter distribution in a sample of ten nearby clusters (0.03 < z < 0.09) with temperatures between 4.7 and 9.4 keV. These galaxy clusters are studied in detail using X-ray data and global physical properties are determined. Correlations between these quantities are analysed and compared with the results for distant clusters. We find an interesting correlation between the extent of the intra-cluster gas relative to the dark matter distribution. The extent of the gas relative to the extent of the dark matter tends to be larger in less massive clusters. This correlation might give us some hints on non-gravitational processes in clusters. We do not see evolution in the gas mass fraction out to a redshift of unity. Within r(500), the mean gas mass fraction obtained is (0.16 +/- 0.02) h(50)(-3/2).Item Discovery of holes in the core of the distant galaxy cluster RBS797 in a CHANDRA observation(tracing cosmic evolution with galaxy clusters, proceeding, 2002) De Filippis, E.; Schindler, S.; Castillo Morales, María África; Schwope, A.; Wambsganss, J.We present CHANDRA X-ray observations of the hot (T = 7.7^(+1.2)_( −1.0), distant (z = 0.354) gakaxy cluster RBS797. The most striking features are two spectacular minima in the X-ray emission in the core of the cluster; this suggests an interaction of radio lobes with the intracluster gas. This is the first time such depressions have been observed in a distant cluster.