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
53 results
Search Results
Now showing 1 - 10 of 53
Item MEGARA: the future IFU and MOS of the 10.4 M GTC(Revista Mexicana de astronomía y astrofísica, 2013) Gil De Paz, Armando; Gallego Maestro, Jesús; Castillo Morales, María África; Eliche Moral, María del Carmen; Marino, Raffaella Anna; Pascual Ramírez, Sergio; Zamorano Calvo, Jaime; Cardiel López, Nicolás; Pérez González, Pablo Guillermo; ... otrosIn these proceedings we summarize the characteristics and current status of MEGARA, the future optical IFU and MOS for the 10.4 m GTC. MEGARA is being built by a Consortium led by the UCM (Spain) that also includes the INAOE (Mexico), the IAA-CSIC (Spain) and the UPM (Spain). The MEGARA IFU offers two different bundles, one called LCB with a field-of-view of 14 x 12 arcsec^2 and a spaxel size of 0.685 arcsec yielding spectral resolutions between R=6000-19000 and another one called SCB covering 10 x 8 arcsec^2 with 0.48 arcsec spaxels and resolutions R=8000-25000. The MOS component allows observing up to 100 targets in 3.5x3.5 arcmin^2. In September 2010 MEGARA was selected as the next optical spectrograph for GTC. Its PDR is scheduled for March 2012 with First Light on 2015.- Project number: 244
Item Prácticas de observaciones astronómicas remotas con telescopios profesionales a través de internet(2017) Gallego Maestro, Jesús; Zamorano Calvo, Jaime; Cardiel López, Nicolás; Castillo Morales, María África; Cacho Martínez, Raúl; Tapia Ayuga, Carlos Eugenio; Pascual Ramírez, Sergio; Pedraz Marcos, SantosEste proyecto se resume como un intento de implementar unas prácticas de laboratorio que permitan llevar a cabo observaciones astronómicas de calidad científica mediante el uso remoto a través de Internet de telescopios profesionales situados en un gran observatorio astronómico. Item Outer-disk reddening and gas-phase metallicities: The CALIFA connection(Astronomy & Astrophysics, 2016) Marino, Raffaella Anna; Gil De Paz, Armando; Sánchez, S. F.; Sánchez Blázquez, Patricia; Cardiel López, Nicolás; Castillo Morales, María África; Pascual Ramírez, Sergio; Vílchez, J.; Kehrig, C.; Mollá, M.; Mendez Abreu, J.; Catalán Torrecilla, Cristina; Florido, E.; Perez, I.; Ruiz Lara, T.; Ellis, S.; López Sánchez, A. R.; González Delgado, R. M.; Lorenzo Cáceres, A. de; García Benito, R.; Galbany, L.; Zibetti, S.; Cortijo, C.; Kalinova, V.; Mast, D.; Iglesias Páramo, J.; Papaderos, P.; Walcher, C. J.; Bland Hawthorn, J.; CALIFA TeamWe study, for the first time in a statistically significant and well-defined sample, the relation between the outer-disk ionized-gas metallicity gradients and the presence of breaks in the surface brightness profiles of disk galaxies. Sloan Digital Sky Survey (SDSS) g′- and r′-band surface brightness, (g′ – r′) color, and ionized-gasoxygen abundance profiles for 324 galaxies within the Calar Alto Legacy Integral Field Area (CALIFA) survey are used for this purpose. We perform a detailed light-profile classification, finding that 84% of our disks show down- or up-bending profiles (Type II and Type III, respectively), while the remaining 16% are well fitted by one single exponential (Type I). The analysis of the color gradients at both sides of this break shows a U-shaped profile for most Type II galaxies with an average minimum (g′ − r′) color of ~0.5 mag and an ionized-gas metallicity flattening associated with it only in the case of low-mass galaxies. Comparatively, more massive systems show a rather uniform negative metallicity gradient. The correlation between metallicity flattening and stellar mass for these systems results in p-values as low as 0.01. Independent of the mechanism having shaped the outer light profiles of these galaxies, stellar migration or a previous episode of star formation in a shrinking star-forming disk, it is clear that the imprint in their ionized-gas metallicity was different for low- and high-mass Type II galaxies. In the case of Type III disks, a positive correlation between the change in color and abundance gradient is found (the null hypothesis is ruled out with a p-value of 0.02), with the outer disks of Type III galaxies with masses ≤10^10 M_⊙ showing a weak color reddening or even a bluing. This is interpreted as primarily due to a mass downsizing effect on the population of Type III galaxies that recently experienced an enhanced inside-out growth.Item The ELT-MOS (MOSAIC): towards the construction phase(Ground-based and airbone instrumentation for astronomy VII, 2018) Gallego Maestro, Jesús; Castillo Morales, María ÁfricaWhen combined with the huge collecting area of the ELT, MOSAIC will be the most effective and flexible Multi-Object Spectrograph (MOS) facility in the world, having both a high multiplex and a multi-Integral Field Unit (Multi-IFU) capability. It will be the fastest way to spectroscopically follow-up the faintest sources, probing the reionisation epoch, as well as evaluating the evolution of the dwarf mass function over most of the age of the Universe. MOSAIC will be world-leading in generating an inventory of both the dark matter (from realistic rotation curves with MOAO fed NIR IFUs) and the cool to warm-hot gas phases in z=3.5 galactic haloes (with visible wavelenth IFUs). Galactic archaeology and the first massive black holes are additional targets for which MOSAIC will also be revolutionary. MOAO and accurate sky subtraction with fibres have now been demonstrated on sky, removing all low Technical Readiness Level (TRL) items from the instrument. A prompt implementation of MOSAIC is feasible, and indeed could increase the robustness and reduce risk on the ELT, since it does not require diffraction limited adaptive optics performance. Science programmes and survey strategies are currently being investigated by the Consortium, which is also hoping to welcome a few new partners in the next two years.Item Three-dimensional spectroscopy of local luminous compact blue galaxies: kinematic maps of a sample of 22 objects(Monthly notices of the Royal Astronomical Society, 2011) Pérez Gallego, J.; Guzmán, R.; Castillo Morales, María África; Gallego Maestro, Jesús; Castander, F. J.; Garland, C. A.; Gruel, N.; Pisano, D. J.; Zamorano Calvo, JaimeWe use three-dimensional optical spectroscopy observations of a sample of 22 local luminous compact blue galaxies (LCBGs) to create kinematic maps. By means of these, we classify the kinematics of these galaxies into three different classes: rotating disc (RD), perturbed rotation (PR) and complex kinematics (CK). We find 48 per cent are RDs, 28 per cent are PRs and 24 per cent are CKs. RDs show rotational velocities that range between similar to 50 and similar to 200 km s(-1), and dynamical masses that range between similar to 1 x 10(9) and similar to 3 x 10(10) M(circle dot). We also address the following two fundamental questions through the study of the kinematic maps: (i) What processes are triggering the current starburst in LCBGs? We search our maps of the galaxy velocity fields for signatures of recent interactions and close companions that may be responsible for the enhanced star formation in our sample. We find that 5 per cent of objects show evidence of a recent major merger, 10 per cent of a minor merger and 45 per cent of a companion. This argues in favour of ongoing interactions with close companions as a mechanism for the enhanced star formation activity in these galaxies. (ii) What processes may eventually quench the current starbust in LCBGs? Velocity and velocity width maps, together with emission line ratio maps, can reveal signatures of active galactic nuclei (AGNs) activity or supernova (SN)-driven galactic winds that could halt the current burst. We find only 5 per cent of objects with clear evidence of AGN activity and 27 per cent with kinematics consistent with SN-driven galactic winds. Therefore, a different mechanism may be responsible for quenching the star formation in LCBGs. Finally, from our analysis, we find that the velocity widths of RDs, rather than accounting exclusively for the rotational nature of these objects, may account as well for other kinematic components and may not be good tracers of their dynamical masses.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.- Project number: PIMCD154/23-24
Item Físicas e ingenieras del mañana: fomentando sus vocaciones científicas(2024) Martín Benito, Mercedes; Castillo Morales, María África; García Payo, M. Carmen; Gómez Nicola, Ángel; Martín Fernández, Fátima; Pérez García, Lucas; Prieto Jiménez, Carlota; Sanmartino Rodríguez, Julio AntonioEste proyecto propone varias iniciativas para fomentar la vocación por la física y las ingenierías que impartimos en la Facultad de CC. Físicas, en alumnas de primaria y secundaria. El objetivo es reducir el desequilibrio de género en nuestro centro.