Zobrazeno 1 - 10
of 75
pro vyhledávání: '"Fernández, N. J."'
Autor:
Gratier, P., Braine, J., Rodriguez-Fernandez, N. J., Schuster, K. F., Kramer, C., Corbelli, E., Combes, F., Brouillet, N., van der Werf, P. P., Röllig, M.
We present an analysis of the systematic CO(2-1) survey at 12" resolution covering most of the local group spiral M 33 which, at a distance of 840 kpc, is close enough that individual giant molecular clouds (GMCs) can be identified. The goal of this
Externí odkaz:
http://arxiv.org/abs/1111.4320
Autor:
Gratier, P., Braine, J., Rodriguez-Fernandez, N. J., Schuster, K. F., Kramer, C., Xilouris, E. M., Tabatabaei, F. S., Henkel, C., Corbelli, E., Israel, F., van der Werf, P. P., Calzetti, D., Garcia-Burillo, S., Sievers, A., Combes, F., Wiklind, T., Brouillet, N., Herpin, F., Bontemps, S., Aalto, S., Koribalski, B., van der Tak, F., Wiedner, M. C., Roellig, M., Mookerjea, B.
We present high resolution large scale observations of the molecular and atomic gas in the Local Group Galaxy M33. The observations were carried out using the HERA at the 30m IRAM telescope in the CO(2-1) line achieving a resolution of 12"x2.6 km/s,
Externí odkaz:
http://arxiv.org/abs/1003.3222
Autor:
Gratier, P., Braine, J., Rodriguez-Fernandez, N. J., Israel, F. P., Schuster, K. F., Brouillet, N., Gardan, E.
Publikováno v:
A&A 512, A68 (2010)
Do molecular clouds collapse to form stars at the same rate in all environments? In large spiral galaxies, the rate of transformation of H2 into stars (hereafter SFE) varies little. However, the SFE in distant objects (z~1) is much higher than in the
Externí odkaz:
http://arxiv.org/abs/1001.5405
Autor:
Rodriguez-Fernandez, N. J.
We discuss the results of the first model of the gas dynamics in the Milky Way in the presence of two bars: the large scale primary bar or boxy bulge and a secondary bar in the Galactic center region. We have obtained an accurate potential by modelin
Externí odkaz:
http://arxiv.org/abs/0901.2066
Autor:
Requena-Torres, M. A., Martín-Pintado, J., Rodríguez-Franco, A., Martín, S., Rodríguez-Fernández, N. J., de Vicente, P.
We study the origin of large abundances of complex organic molecules in the Galactic center (GC). We carried out a systematic study of the complex organic molecules CH3OH, C2H5OH, (CH3)2O, HCOOCH3, HCOOH, CH3COOH, H2CO, and CS toward 40 GC molecular
Externí odkaz:
http://arxiv.org/abs/astro-ph/0605031
The CII 158 microns line is the most important coolant of the interstellar medium in galaxies but substantial variations are seen from object to object. The main source of the emission at a galactic scale is still poorly understood. Previous studies
Externí odkaz:
http://arxiv.org/abs/astro-ph/0603423
Publikováno v:
Space Science Reviews 2005
An overview is given of ISO results on regions of high excitation ISM and gas, i.e. HII regions, the Galactic Centre and Supernovae Remnants. IR emission due to fine-structure lines, molecular hydrogen, silicates, polycyclic aromatic hydrocarbons and
Externí odkaz:
http://arxiv.org/abs/astro-ph/0503711
Publikováno v:
Astron.Astrophys. 429 (2005) 923-938
(Abridged) We present fine structure and recombination lines observations of the ionized gas toward a sample of 18 sources located within 300 pc of the center of the Galaxy (GC). The fine structure lines from [NII] and [SIII] have been detected in 16
Externí odkaz:
http://arxiv.org/abs/astro-ph/0409334
Publikováno v:
Astron.Astrophys. 427 (2004) 217-229
The 500 central pc of the Galaxy (hereafter GC) exhibit a widespread gas component with a kinetic temperature of 100-200 K. The bulk of this gas is not associated to the well-known thermal radio continuum or far infrared sources like Sgr A or Sgr B.
Externí odkaz:
http://arxiv.org/abs/astro-ph/0407479
Publikováno v:
Astron.Astrophys. 419 (2004) 897-912
There is observational evidence that nuclear winds and X-rays can heavily influence the physical conditions and chemical abundances of molecular gas in the circumnuclear disks (CND) of Active Galactic Nuclei (AGN). In this paper we probe the chemical
Externí odkaz:
http://arxiv.org/abs/astro-ph/0402556