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
32 results
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Now showing 1 - 10 of 32
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 3D spectroscopy of local luminous compact blue galaxies: kinematics of NGC 7673(Monthly notices of the Royal Astronomical Society, 2010) Pérez Gallego, J.; Guzmán, R.; Castillo Morales, María África; Castander, F. J.; Gallego Maestro, Jesús; Garland, C. A.; Gruel, N.; Pisano, D. J.; Sánchez, S. F.; Zamorano Calvo, JaimeThe kinematic properties of the ionized gas of local luminous compact blue galaxy NGC 7673 are presented using three-dimensional data taken with the PPAK integral field unit at the 3.5-m telescope in the Centro Astronomico Hispano Aleman. Our data reveal an asymmetric rotating velocity field with a peak-to-peak difference of 60 km s(-1). The kinematic centre is found to be at the position of a central velocity width maximum (sigma = 54 +/- 1 kms(-1)), which is consistent with the position of the luminosity-weighted centroid of the entire galaxy. The position angle of the minor rotation axis is 168 degrees as measured from the orientation of the velocity field contours. At least two decoupled kinematic components are found. The first one is compact and coincides with the position of the second most active star formation region (clump B). The second one is extended and does not have a clear optical counterpart. No evidence of active galactic nuclei activity or supernovae galactic winds powering any of these two components has been found. Our data, however, show evidence in support of a previously proposed minor merger scenario in which a dwarf galaxy, tentatively identified with clump B, is falling into NGC 7673 and triggers the starburst. Finally, it is shown that the dynamical mass of this galaxy may be severely underestimated when using the derived rotation curve or the integrated velocity width, under the assumption of virialization.Item Blasts and shocks in the disc of NGC 4258(Monthly notices of the Royal Astronomical Society, 2010) Jiménez Vicente, J.; Mediavilla, E.; Castillo Morales, María África; Battaner, E.We present integral field spectroscopic observations of the central region of the active galaxy NGC 4258 obtained with the fibre IFU system INTEGRAL. We have been able to detect cold neutral gas by means of the interstellar NaD doublet absorption and to trace its distribution and kinematics with respect to the underlying disc. The neutral gas is blueshifted with projected velocities in the 120-370 km s(-1) range. We have also detected peculiar kinematics in part of the ionized gas in this region by means of a careful kinematic decomposition. The bipolar spatial distribution of the broader component is roughly coincident with the morphology of the X-ray diffuse emission. The kinematics of this gas can be explained in terms of expansion at very high (projected) velocities of up to 300 km s(-1). The observations also reveal the existence of a strip of neutral gas, parallel to the major kinematic axis, that is nearly coincident with a region of very high [S II]/H alpha ratio tracing the shocked gas. Our observations are consistent with the jet model presented by Wilson, Yang & Cecil in which a cocoon originating from the nuclear jet is shocking the gas in the galaxy disc. Alternatively, our observations are also consistent with the bipolar hypershell model of Sofue and Sofue & Vogler. On balance, we prefer the latter model as the most likely explanation for the puzzling features of this peculiar object.- Project number: 54
Item Fomento del uso de software libre de tipo científico en estudios de ciencias(2015) Franco Peláez, Francisco Javier; Antoranz Canales, Pedro; Castillo Morales, María África; García Payo, M. Carmen; Olea Ariza, JavierIncidencias en la creación de una base de dato online de software científico de uso gratuito para alumnos de las titulaciones de la Facultada de Físicas Item Integral field spectroscopy of local LCBGs: NGC 7673, a case study. Physical properties of star-forming regions(Monthly notices of the Royal Astronomical Society, 2011) Castillo Morales, María África; Gallego Maestro, Jesús; Pérez Gallego, J.; Guzmán, R.; Muñoz Mateos, J. C.; Zamorano Calvo, Jaime; Sánchez, S. F.Physical properties of the star-forming regions in the local Luminous Compact Blue Galaxy (LCBG) NGC 7673 are studied in detail using 3D spectroscopic data taken with the PMAS fibre pack (PPAK) integral field unit at the 3.5-m telescope in the Centro Astronomico Hispano Aleman (CAHA). We derive integrated and spatially resolved properties such as extinction, star formation rate (SFR) and metallicity for this galaxy. Our data show an extinction map with maximum values located at the position of the main clumps of star formation showing small spatial variations [E(B - V)(t) = 0.12-0.21 mag]. We derive an H alpha-based SFR for this galaxy of 6.2 +/- 0.8M(circle dot) yr(-1) in agreement with the SFR derived from infrared and radio continuum fluxes. The star formation is located mainly in clumps A, B, C and F. Different properties measured in clump B make this region peculiar. We find the highest H alpha luminosity with an SFR surface density of 0.5 M-circle dot yr(-1) kpc(-2) in this clump. In our previous work, the kinematic analysis for this galaxy shows an asymmetrical ionized gas velocity field with a kinematic decoupled component located at the position of clump B. This region shows the absence of strong absorption features and the presence of a Wolf-Rayet stellar population indicating that this is a young burst of massive stars. Furthermore, we estimate a gas metallicity of 12 + log(O/H) = 8.20 +/- 0.15 (0.32 solar) for the integrated galaxy using the R23 index. The values derived for the different clumps with this method show small metallicity variations in this galaxy, with values in the range 8.12 (for clump A) to 8.23 (for clump B) for 12 + log(O/H). The analysis of the emission-line ratios discards the presence of any active galactic nuclei (AGN) activity or shocks as the ionization source in this galaxy. Between the possible mechanisms to explain the starburst activity in this galaxy, our 3D spectroscopic data support the scenario of an on-going interaction with the possibility for clump B to be the dwarf satellite galaxy.Item The multiphase starburst-driven galactic wind in NGC 5394(Monthly notices of the Royal Astronomical Society, 2016) Martín Fernández, Pablo; Jiménez Vicente, Jorge; Zurita, Almudena; Mediavilla, Evencio; Castillo Morales, María ÁfricaWe present a detailed study of the neutral and ionized gas phases in the galactic wind for the nearby starburst galaxy NGC 5394 based on new integral field spectroscopy obtained with the INTEGRAL fibre system at the William Herschel Telescope. The neutral gas phase in the wind is detected via the interstellar Na I D doublet absorption. After a careful removal of the stellar contribution to these lines, a significant amount of neutral gas (∼10^7 M_⊙) is detected in a central region of ∼1.75 kpc size. This neutral gas is blueshifted by ∼165 km s^−1 with respect to the underlying galaxy. The mass outflow of neutral gas is comparable to the star formation rate of the host galaxy. Simultaneously, several emission lines (Hα, [N II], [S II]) are also analysed looking for the ionized warm phase counterpart of the wind. A careful kinematic decomposition of the line profiles reveals the presence of a secondary, broader, kinematic component. This component is found roughly in the same region where the Na I D absorption is detected. It presents higher [N II]/Hα and [S II]/Hα line ratios than the narrow component at the same locations, indicative of contamination by shock ionization. This secondary component also presents blueshifted velocities, although smaller than those measured for the neutral gas, averaging to ∼−30 km s^−1. The mass and mass outflow rate of the wind is dominated by the neutral gas, of which a small fraction might be able to escape the gravitational potential of the host galaxy. The observations in this system can be readily understood within a bipolar gas flow scenario.