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Your search keyword '"Cerviño, M."' showing total 18 results
Start Over Author "Cerviño, M." Journal monthly notices of the royal astronomical society
18 results on '"Cerviño, M."'

2. new reference catalogue for the very metal-poor Universe: +150 OB stars in Sextans A.

Author

Lorenzo, M, Garcia, M, Najarro, F, Herrero, A, Cerviño, M, and Castro, N

Subjects
SMALL magellanic cloud, UNIVERSE, GALACTIC evolution, SUPERGIANT stars, GALACTIC halos, CATALOGS, CATALOGING
Abstract

Local Group (LG) very metal-poor massive stars are the best proxy for the First Stars of the Universe and fundamental to modelling the evolution of early galaxies. These stars may follow new evolutionary pathways restricted to very low metallicities, such as chemically homogeneous evolution (CHE). However, given the great distance leap needed to reach very metal-poor galaxies of the LG and vicinity, no comprehensive spectroscopic studies have been carried out at metallicities lower than the Small Magellanic Cloud (SMC; Z = 1/5 Z⊙) until now. After five observing campaigns at the 10.4-m Gran Telescopio Canarias, we have assembled a low-resolution (R ∼ 1000) spectroscopic collection of more than 150 OB stars in the 1/10 Z⊙ galaxy Sextans A, increasing by an order of magnitude the number of massive stars known in this galaxy. The catalogue includes 38 BA-type supergiants, four red supergiants, and the first candidate 1/10 Z⊙ binary systems, CHE sources and systems hosting stripped stars. The sample massive stars mainly overlap the higher concentrations of neutral gas of Sextans A. However, we find some sources in low H  i column-density regions. The colour–magnitude diagram of the galaxy presents large dispersion, which suggests uneven, internal extinction in Sextans A. This is the largest catalogue of OB-type stars ever produced at sub-SMC metallicities. This sample constitutes a fundamental first step to unveiling the evolutionary pathways and fates of very metal-poor massive stars, analyzing the dependence of radiation-driven winds with metallicity, and studying binary systems in an environment analogue to the early Universe. [ABSTRACT FROM AUTHOR]

Published
2022
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7. AKs-band-selected catalogue of objects in the ALHAMBRA survey

Author

Nieves-Seoane, L., primary, Fernandez-Soto, A., additional, Arnalte-Mur, P., additional, Molino, A., additional, Stefanon, M., additional, Ferreras, I., additional, Ascaso, B., additional, Ballesteros, F. J., additional, Cristóbal-Hornillos, D., additional, López-Sanjuán, C., additional, Hurtado-Gil, Ll., additional, Márquez, I., additional, Masegosa, J., additional, Aguerri, J. A. L., additional, Alfaro, E., additional, Aparicio-Villegas, T., additional, Benítez, N., additional, Broadhurst, T., additional, Cabrera-Caño, J., additional, Castander, F. J., additional, Cepa, J., additional, Cerviño, M., additional, González Delgado, R. M., additional, Husillos, C., additional, Infante, L., additional, Martínez, V. J., additional, Moles, M., additional, Olmo, A. del, additional, Perea, J., additional, Pović, M., additional, Prada, F., additional, Quintana, J. M., additional, Troncoso-Iribarren, P., additional, and Viironen, K., additional

Published
2016
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8. The impact from survey depth and resolution on the morphological classification of galaxies

Author

Pović, M., primary, Márquez, I., additional, Masegosa, J., additional, Perea, J., additional, Olmo, A. del, additional, Simpson, C., additional, Aguerri, J. A. L., additional, Ascaso, B., additional, Jiménez-Teja, Y., additional, López-Sanjuan, C., additional, Molino, A., additional, Pérez-García, A. M., additional, Viironen, K., additional, Husillos, C., additional, Cristóbal-Hornillos, D., additional, Caldwell, C., additional, Benítez, N., additional, Alfaro, E., additional, Aparicio-Villegas, T., additional, Broadhurst, T., additional, Cabrera-Caño, J., additional, Castander, F. J., additional, Cepa, J., additional, Cerviño, M., additional, Fernández-Soto, A., additional, Delgado, R. M. González, additional, Infante, L., additional, Martínez, V. J., additional, Moles, M., additional, Prada, F., additional, and Quintana, J. M., additional

Published
2015
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9. Galaxy clusters and groups in the ALHAMBRA survey

Author

Ascaso, B., primary, Benítez, N., additional, Fernández-Soto, A., additional, Arnalte-Mur, P., additional, López-Sanjuan, C., additional, Molino, A., additional, Schoenell, W., additional, Jiménez-Teja, Y., additional, Merson, A. I., additional, Huertas-Company, M., additional, Díaz-García, L. A., additional, Martínez, V. J., additional, Cenarro, A. J., additional, Dupke, R., additional, Márquez, I., additional, Masegosa, J., additional, Nieves-Seoane, L., additional, Pović, M., additional, Varela, J., additional, Viironen, K., additional, Aguerri, J.A.L., additional, Olmo, A. Del, additional, Moles, M., additional, Perea, J., additional, Alfaro, E., additional, Aparicio-Villegas, T., additional, Broadhurst, T., additional, Cabrera-Caño, J., additional, Castander, F. J., additional, Cepa, J., additional, Cerviño, M., additional, Delgado, R. M. González, additional, Cristóbal-Hornillos, D., additional, Hurtado-Gil, L., additional, Husillos, C., additional, Infante, L., additional, Prada, F., additional, and Quintana, J. M., additional

Published
2015
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10. The ALHAMBRA Survey: Bayesian photometric redshifts with 23 bands for 3 deg2

Author

Molino, A., primary, Benítez, N., additional, Moles, M., additional, Fernández-Soto, A., additional, Cristóbal-Hornillos, D., additional, Ascaso, B., additional, Jiménez-Teja, Y., additional, Schoenell, W., additional, Arnalte-Mur, P., additional, Pović, M., additional, Coe, D., additional, López-Sanjuan, C., additional, Díaz-García, L. A., additional, Varela, J., additional, Stefanon, M., additional, Cenarro, J., additional, Matute, I., additional, Masegosa, J., additional, Márquez, I., additional, Perea, J., additional, Del Olmo, A., additional, Husillos, C., additional, Alfaro, E., additional, Aparicio-Villegas, T., additional, Cerviño, M., additional, Huertas-Company, M., additional, Aguerri, J. A. L., additional, Broadhurst, T., additional, Cabrera-Caño, J., additional, Cepa, J., additional, González, R. M., additional, Infante, L., additional, Martínez, V. J., additional, Prada, F., additional, and Quintana, J. M., additional

Published
2014
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11. The ALHAMBRA survey: evolution of galaxy clustering since z ∼ 1

Author

Arnalte-Mur, P., primary, Martínez, V. J., additional, Norberg, P., additional, Fernández-Soto, A., additional, Ascaso, B., additional, Merson, A. I., additional, Aguerri, J. A. L., additional, Castander, F. J., additional, Hurtado-Gil, L., additional, López-Sanjuan, C., additional, Molino, A., additional, Montero-Dorta, A. D., additional, Stefanon, M., additional, Alfaro, E., additional, Aparicio-Villegas, T., additional, Benítez, N., additional, Broadhurst, T., additional, Cabrera-Caño, J., additional, Cepa, J., additional, Cerviño, M., additional, Cristóbal-Hornillos, D., additional, del Olmo, A., additional, González Delgado, R. M., additional, Husillos, C., additional, Infante, L., additional, Márquez, I., additional, Masegosa, J., additional, Moles, M., additional, Perea, J., additional, Pović, M., additional, Prada, F., additional, and Quintana, J. M., additional

Published
2014
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12. The ALHAMBRA survey: reliable morphological catalogue of 22 051 early- and late-type galaxies

Author

Pović, M., primary, Huertas-Company, M., additional, Aguerri, J. A. L., additional, Márquez, I., additional, Masegosa, J., additional, Husillos, C., additional, Molino, A., additional, Cristóbal-Hornillos, D., additional, Perea, J., additional, Benítez, N., additional, Olmo, A. del, additional, Fernández-Soto, A., additional, Jiménez-Teja, Y., additional, Moles, M., additional, Alfaro, E., additional, Aparicio-Villegas, T., additional, Ascaso, B., additional, Broadhurst, T., additional, Cabrera-Caño, J., additional, Castander, F. J., additional, Cepa, J., additional, Fernandez Lorenzo, M., additional, Cerviño, M., additional, Delgado, R. M. González, additional, Infante, L., additional, López-Sanjuan, C., additional, Martínez, V. J., additional, Matute, I., additional, Oteo, I., additional, Pérez-García, A. M., additional, Prada, F., additional, and Quintana, J. M., additional

Published
2013
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13. Lyman Break and ultraviolet-selected galaxies at z ∼ 1 – II. PACS 100 μm/160 μm FIR detections★

Author

Oteo, I., primary, Magdis, G., additional, Bongiovanni, Á., additional, Pérez-García, A. M., additional, Cepa, J., additional, Cedrés, B., additional, Ederoclite, A., additional, Sánchez-Portal, M., additional, Aguerri, J. A. L., additional, Alfaro, E. J., additional, Altieri, B., additional, Andreani, P., additional, Aparicio-Villegas, T., additional, Aussel, H., additional, Benítez, N., additional, Berta, S., additional, Broadhurst, T., additional, Cabrera-Caño, J., additional, Castander, F. J., additional, Cerviño, M., additional, Cimatti, A., additional, Cristobal-Hornillos, D., additional, Daddi, E., additional, Elbaz, D., additional, Fernandez-Soto, A., additional, Schreiber, N. Förster, additional, Genzel, R., additional, Gonzalez-Delgado, R. M., additional, Husillos, C., additional, Infante, L., additional, Le Floc'h, E., additional, Lutz, D., additional, Magnelli, B., additional, Maiolino, R., additional, Márquez, I., additional, Martínez, V. J., additional, Masegosa, J., additional, Matute, I., additional, Moles, M., additional, Molino, A., additional, Olmo, A. del, additional, Perea, J., additional, Pérez-Martínez, R., additional, Pintos-Castro, I., additional, Poglitsch, A., additional, Polednikova, J., additional, Popesso, P., additional, Pović, M., additional, Pozzi, F., additional, Prada, F., additional, Quintana, J. M., additional, Riguccini, L., additional, Sturm, E., additional, Tacconi, L., additional, Valtchanov, I., additional, and Viironen, K., additional

Published
2013
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14. Lyman break and ultraviolet-selected galaxies at z ∼ 1 – I. Stellar populations from the ALHAMBRA survey

Author

Oteo, I., primary, Bongiovanni, Á., additional, Cepa, J., additional, Pérez-García, A. M., additional, Ederoclite, A., additional, Sánchez-Portal, M., additional, Pintos-Castro, I., additional, Pérez-Martínez, R., additional, Polednikova, J., additional, Aguerri, J. A. L., additional, Alfaro, E. J., additional, Aparicio-Villegas, T., additional, Benítez, N., additional, Broadhurst, T., additional, Cabrera-Caño, J., additional, Castander, F. J., additional, Cerviño, M., additional, Cristobal-Hornillos, D., additional, Fernandez-Soto, A., additional, Gonzalez-Delgado, R. M., additional, Husillos, C., additional, Infante, L., additional, Martínez, V. J., additional, Márquez, I., additional, Masegosa, J., additional, Matute, I., additional, Moles, M., additional, Molino, A., additional, Olmo, A. del, additional, Perea, J., additional, Pović, M., additional, Prada, F., additional, Quintana, J. M., additional, and Viironen, K., additional

Published
2013
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17. Nebular and stellar properties of a metal-poor H iigalaxy atz= 3.36.

Author

Villar-Martín, M., Cerviño, M., and Delgado, R. M. González

Subjects
*STAR formation, *TEMPERATURE of stars, *PARTICLES (Nuclear physics), *PHOTOCHEMISTRY, *NITROGEN, *IONIZED gases
Abstract

We have characterized the physical properties (electron temperature, density and metallicity) of the ionized gas and the ionizing population (age, metallicity and presence of Wolf–Rayet stars) in the Lynx arc, an H iigalaxy at. The ultraviolet doublets (i.e. C iii], Si iii] and N iv) imply the existence of a density gradient in this object, with a high-density regionand a lower density region (<3200 cm−3). The temperature-sensitive ratio[O iii]λλ1661,1666/λ5007 implies an electron temperature, in agreement within the errors with photoionization model predictions. Nebular abundance determination using standard techniques and the results from photoionization models imply a nebular metallicity of, in good agreement with recent results from Fosbury et al. Both methods suggest that nitrogen is overabundant relative to other elements, with. We do not find evidence for Si overabundance, as Fosbury et al. did.Photoionization models imply that the ionizing stellar population in the Lynx arc has an age of≲5 Myr. If He+ is ionized by Wolf–Rayet (WR) stars, then the ionizing stars in the Lynx arc have metallicitiesand ages∼2.8–3.4 Myr (depending onZstar), when WR stars appear and are responsible for theemission. However, alternative excitation mechanisms for this species are not discarded. Since the emission lines trace the properties of the present burst only, nothing can be said about the possible presence of an underlying old stellar population.The Lynx arc is a low-metallicity H iigalaxy that is undergoing a burst of star formation of≲5 Myr age. One possible scenario that explains the emission-line spectrum of the Lynx arc, the large strength of the nitrogen lines and theemission is that the object has experienced a merger event that has triggered a burst of star formation. WR stars have formed that contribute to a fast enrichment of the interstellar medium.Like Fosbury et al., we find a factor of≳10 discrepancy between the mass of the instantaneous burst required to power the luminosity of the Hβ line and the mass implied by the continuum level measured for the Lynx arc. We discuss several possible solutions to this problem. The most likely explanation is that gas and stars have different spatial distributions, so that the emission lines and the stellar continuum suffer different gravitational amplifications by the intervening cluster. [ABSTRACT FROM AUTHOR]

Published
2004
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18. On biases in the predictions of stellar population synthesis models.

Author

Cerviño, M. and Valls-Gabaud, D.

Subjects
*STELLAR populations, *STATISTICS
Abstract

Sampling fluctuations in stellar populations give rise to dispersion in observables when a small number of sources contribute effectively to the observables. This is the case for a variety of linear functions of the spectral energy distribution (SED) in small stellar systems, such as galactic and extragalactic HII regions, dwarf galaxies or stellar clusters. In this paper we show that sampling fluctuations also introduce systematic biases and multimodality in non-linear functions of the SED, such as luminosity ratios, magnitudes and colours. In some cases, the distribution functions of rational and logarithmic quantities are bimodal, hence complicating the interpretation of these quantities considerably in terms of age or evolutionary stages. These biases can only be assessed by Monte Carlo simulations. We find that biases are usually negligible when the effective number of stars, N, which contribute to a given observable is larger than 10. Bimodal distributions may appear when N is between 10 and 0.1. Predictions from any model of stellar population synthesis become extremely unreliable for small N values, providing an operational limit to the applicability of such models for the interpretation of integrated properties of stellar systems. In terms of stellar masses, assuming a Salpeter initial mass function in the range 0.08-120 M⊙, N = 10 corresponds to about 10[sup 5] M⊙ (although the exact value depends on the age and the observable). This bias may account, at least in part, for claimed variations in the properties of the stellar initial mass function in small systems, and arises from the discrete nature of small stellar populations. [ABSTRACT FROM AUTHOR]

Published
2003
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