Since the generation of the first stars (see Sect. 9.6) massive star-formation has been the major... more Since the generation of the first stars (see Sect. 9.6) massive star-formation has been the major driver in the evolution of the universe as we know it today. Massive stars are the factories that produce elements up to iron during their lifetimes and enrich the ISM with heavy trace elements during their supernova phases. Furthermore their UV radiation, stellar winds, and explosive deaths deposit much of the energy and turbulence into the ISM we see today. Even though massive stars are comparatively rare at a given time according to the IMF (see Fig. 3.27) their average lifetime of a few Myr (see Eqn. 2.2) makes them very efficient element manufacturers. During the Sun’s lifetime of 8 Gyr, massive stars will have enriched a few \\(1{0}^{4}{M}_{\\odot }\\)by many orders of magnitude if we assume an average mass of \\(20{M}_{\\odot }\\)for each star. In that respect massive stars dominate the total energy output of galaxies as well as the energy balance in the ISM (see Chap. 3).
Peimbert (2001). Fig. 2. Upper panel: H# brightness profile of the best-fit model (solid line), c... more Peimbert (2001). Fig. 2. Upper panel: H# brightness profile of the best-fit model (solid line), compared to the observed profile by Castaneda et al. (1992) (dot-dashed line). Lower panel: I(# 6717)/I(# 6731) ratio profile of the best-fit model, superposed to the observational data by Castaneda et al. (1992) (asterisks). REFERENCES
line ratios obtained earlier are used in this process. To calculate the T e and N e the user has ... more line ratios obtained earlier are used in this process. To calculate the T e and N e the user has to provide a line ratio 1 Facultad de Ciencias, UABC, Ensenada, Mexico. Instituto de Astronoma, UNAM, Ensenada, Mexico. Fig. 1. Screenshot of xAbIon. (from [O III] or [N II] to calculate the temperature and [S II] for density), the energy level transitions and an initial value for the N e or the T e , respectively. After obtaining the T e and N e , the ion abundances by number for each ion can be calculated. First, the ionic abundance ratio is estimated and recognized automatically by the system. Then, the ionic abundances by number can be calculated. This process is repeated until the ionic abundances for all the ions are computed. Both the first and second phase write the results in a L A T E X formatted file. The file written by xGalRed contains a table with the ions, their wavelength, observed and dereddened fluxes and the extinction law. xAbIon write its results in the corres
Proceedings of the International Astronomical Union, 2009
In de la Fuente (2007; Ph. D. Thesis), the molecular clump associated with the ultracompact HII r... more In de la Fuente (2007; Ph. D. Thesis), the molecular clump associated with the ultracompact HII region G12.21–0.10 was confirmed as a large, hot, dense Hot Molecular Core nearby to the ionized gas. The density was confirmed by comparing low resolution NH3(2, 2) and (4, 4) VLA observations, with other molecular lines and radio–continuum observations. These results will be presented in detail in a forthcoming paper (de la Fuente et al. in preparation). In these works, for the first time, the spatial location of the Hot Molecular Core is presented. Here we present the NH3(4,4) observations from de la Fuente (2007; Ph. D. Thesis), confirming that the hotter and denser gas in the molecular core lies in a compact structure, of smaller scale than the NH3(2, 2) emission.
Proceedings of the International Astronomical Union, 2006
The Virtual Solar Observatory (VSO) concept outlines a software environment for searching, obtain... more The Virtual Solar Observatory (VSO) concept outlines a software environment for searching, obtaining and analyzing data from archives of solar data that are distributed at many different observatories around the world (Hill 2006, in this volume). The VSO, however, not only provides fast and reliable access to the existing data of Solar Active Regions, but also represents a powerful and unique tool to perform numerical simulations of the evolution and present state of solar phenomena. Two centers at UNAM, the Institute of Astronomy (IA) and the Supercomputer Center (DGSCA), along with the Sonora University, are working together to create the Mexican Virtual Solar Observatory (MVSO) that will be part of a wider national effort.
Abstract: We are proposing to conduct a multicolor, synoptic infrared (IR) imaging survey of the ... more Abstract: We are proposing to conduct a multicolor, synoptic infrared (IR) imaging survey of the Northern sky with a new, dedicated 6.5-meter telescope at San Pedro M\'artir (SPM) Observatory. This initiative is being developed in partnership with astronomy institutions in Mexico and the University of California. The 4-year, dedicated survey, planned to begin in 2017, will reach more than 100 times deeper than 2MASS. The Synoptic All-Sky Infrared (SASIR) Survey will reveal the missing sample of faint red dwarf stars in the local solar ...
We are proposing to conduct a simultaneous multicolor (Y, J, H, K) synoptic infrared (IR) imaging... more We are proposing to conduct a simultaneous multicolor (Y, J, H, K) synoptic infrared (IR) imaging survey of the entire sky (above declination δ = −30 ◦ ) with a new, dedicated 6.5-meter telescope at San Pedro Mártir (SPM) Observatory (Mexico). This initiative is being developed in partnership with astronomy institutions in Mexico, the University of California, and the University of Arizona. This 4–5 year, dedicated survey, planned to begin in 2017, will reach more than 100 times deeper than 2MASS [27], increasing the effective detection volume by more than one
Since the generation of the first stars (see Sect. 9.6) massive star-formation has been the major... more Since the generation of the first stars (see Sect. 9.6) massive star-formation has been the major driver in the evolution of the universe as we know it today. Massive stars are the factories that produce elements up to iron during their lifetimes and enrich the ISM with heavy trace elements during their supernova phases. Furthermore their UV radiation, stellar winds, and explosive deaths deposit much of the energy and turbulence into the ISM we see today. Even though massive stars are comparatively rare at a given time according to the IMF (see Fig. 3.27) their average lifetime of a few Myr (see Eqn. 2.2) makes them very efficient element manufacturers. During the Sun’s lifetime of 8 Gyr, massive stars will have enriched a few \\(1{0}^{4}{M}_{\\odot }\\)by many orders of magnitude if we assume an average mass of \\(20{M}_{\\odot }\\)for each star. In that respect massive stars dominate the total energy output of galaxies as well as the energy balance in the ISM (see Chap. 3).
Peimbert (2001). Fig. 2. Upper panel: H# brightness profile of the best-fit model (solid line), c... more Peimbert (2001). Fig. 2. Upper panel: H# brightness profile of the best-fit model (solid line), compared to the observed profile by Castaneda et al. (1992) (dot-dashed line). Lower panel: I(# 6717)/I(# 6731) ratio profile of the best-fit model, superposed to the observational data by Castaneda et al. (1992) (asterisks). REFERENCES
line ratios obtained earlier are used in this process. To calculate the T e and N e the user has ... more line ratios obtained earlier are used in this process. To calculate the T e and N e the user has to provide a line ratio 1 Facultad de Ciencias, UABC, Ensenada, Mexico. Instituto de Astronoma, UNAM, Ensenada, Mexico. Fig. 1. Screenshot of xAbIon. (from [O III] or [N II] to calculate the temperature and [S II] for density), the energy level transitions and an initial value for the N e or the T e , respectively. After obtaining the T e and N e , the ion abundances by number for each ion can be calculated. First, the ionic abundance ratio is estimated and recognized automatically by the system. Then, the ionic abundances by number can be calculated. This process is repeated until the ionic abundances for all the ions are computed. Both the first and second phase write the results in a L A T E X formatted file. The file written by xGalRed contains a table with the ions, their wavelength, observed and dereddened fluxes and the extinction law. xAbIon write its results in the corres
Proceedings of the International Astronomical Union, 2009
In de la Fuente (2007; Ph. D. Thesis), the molecular clump associated with the ultracompact HII r... more In de la Fuente (2007; Ph. D. Thesis), the molecular clump associated with the ultracompact HII region G12.21–0.10 was confirmed as a large, hot, dense Hot Molecular Core nearby to the ionized gas. The density was confirmed by comparing low resolution NH3(2, 2) and (4, 4) VLA observations, with other molecular lines and radio–continuum observations. These results will be presented in detail in a forthcoming paper (de la Fuente et al. in preparation). In these works, for the first time, the spatial location of the Hot Molecular Core is presented. Here we present the NH3(4,4) observations from de la Fuente (2007; Ph. D. Thesis), confirming that the hotter and denser gas in the molecular core lies in a compact structure, of smaller scale than the NH3(2, 2) emission.
Proceedings of the International Astronomical Union, 2006
The Virtual Solar Observatory (VSO) concept outlines a software environment for searching, obtain... more The Virtual Solar Observatory (VSO) concept outlines a software environment for searching, obtaining and analyzing data from archives of solar data that are distributed at many different observatories around the world (Hill 2006, in this volume). The VSO, however, not only provides fast and reliable access to the existing data of Solar Active Regions, but also represents a powerful and unique tool to perform numerical simulations of the evolution and present state of solar phenomena. Two centers at UNAM, the Institute of Astronomy (IA) and the Supercomputer Center (DGSCA), along with the Sonora University, are working together to create the Mexican Virtual Solar Observatory (MVSO) that will be part of a wider national effort.
Abstract: We are proposing to conduct a multicolor, synoptic infrared (IR) imaging survey of the ... more Abstract: We are proposing to conduct a multicolor, synoptic infrared (IR) imaging survey of the Northern sky with a new, dedicated 6.5-meter telescope at San Pedro M\'artir (SPM) Observatory. This initiative is being developed in partnership with astronomy institutions in Mexico and the University of California. The 4-year, dedicated survey, planned to begin in 2017, will reach more than 100 times deeper than 2MASS. The Synoptic All-Sky Infrared (SASIR) Survey will reveal the missing sample of faint red dwarf stars in the local solar ...
We are proposing to conduct a simultaneous multicolor (Y, J, H, K) synoptic infrared (IR) imaging... more We are proposing to conduct a simultaneous multicolor (Y, J, H, K) synoptic infrared (IR) imaging survey of the entire sky (above declination δ = −30 ◦ ) with a new, dedicated 6.5-meter telescope at San Pedro Mártir (SPM) Observatory (Mexico). This initiative is being developed in partnership with astronomy institutions in Mexico, the University of California, and the University of Arizona. This 4–5 year, dedicated survey, planned to begin in 2017, will reach more than 100 times deeper than 2MASS [27], increasing the effective detection volume by more than one
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Papers by José Franco