The herschel virgo cluster survey: X. the relationship between cold dust and molecular gas content in Virgo spirals
Por:
Corbelli E., Bianchi S., Cortese L., Giovanardi C., Magrini L., Pappalardo C., Boselli A., Bendo G.J., Davies J., Grossi M., Madden S.C., Smith M.W.L., Vlahakis C., Auld R., Baes M., De Looze I., Fritz J., Pohlen M., Verstappen J.
Publicada:
1 ene 2012
Resumen:
Aims. We examine whether dust mass can trace the total or molecular gas mass in late-type Virgo cluster galaxies, and how the environment affects the dust-to-gas ratio and the molecular fraction. Methods. Using the far-infrared emission, as observed by the Herschel Virgo Cluster Survey (HeViCS), and the integrated HI 21-cm and CO J = 1-0 line brightness, we infer the dust and total gas mass for a magnitude limited sample of 35 metal rich spiral galaxies. Environmental disturbances on each galaxy are considered by means of the HI deficiency parameter. Results. The CO flux correlates tightly and linearly with far-infrared fluxes observed by Herschel, especially with the emission at 160, 250 and 350 µm. Molecules in these galaxies are more closely related to cold dust rather than to dust heated by star formation or to optical/NIR brightness. We show that dust mass establishes a stronger correlation with the total gas mass than with the atomic or molecular component alone. The correlation is non-linear since lower mass galaxies have a lower dust-to-gas ratio. The dust-to-gas ratio increases as the HI deficiency increases, but in highly HI deficient galaxies it stays constant. Dust is in fact less affected than atomic gas by weak cluster interactions, which remove most of the HI gas from outer and high latitudes regions. Highly disturbed galaxies, in a dense cluster environment, can instead loose a considerable fraction of gas and dust from the inner regions of the disk keeping constant the dust-to-gas ratio. There is evidence that the molecular phase is also quenched. This quencing becomes evident by considering the molecular gas mass per unit stellar mass. Its amplitude, if confirmed by future studies, highlights that molecules are missing in Virgo HI deficient spirals, but to a somewhat lesser extent than dust. © 2012 ESO.
Filiaciones:
Corbelli E.:
Osservatorio Astrofisico di Arcetri, INAF, Largo E. Fermi 5, 50125 Firenze, Italy
Bianchi S.:
Osservatorio Astrofisico di Arcetri, INAF, Largo E. Fermi 5, 50125 Firenze, Italy
Cortese L.:
European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei Munchen, Germany
Giovanardi C.:
Osservatorio Astrofisico di Arcetri, INAF, Largo E. Fermi 5, 50125 Firenze, Italy
Magrini L.:
Osservatorio Astrofisico di Arcetri, INAF, Largo E. Fermi 5, 50125 Firenze, Italy
Pappalardo C.:
Osservatorio Astrofisico di Arcetri, INAF, Largo E. Fermi 5, 50125 Firenze, Italy
Boselli A.:
Laboratoire d'Astrophysique de Marseille, UMR 6110 CNRS, 38 rue F. Joliot-Curie, 13388 Marseille, France
Bendo G.J.:
Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Manchester M13 9PL, United Kingdom
Davies J.:
Department of Physics and Astronomy, Cardiff University, Parade, Cardiff, CF24 3AA, United Kingdom
Grossi M.:
CAAUL, Observatorio Astronomico de Lisboa, Universidade de Lisboa, Tapada de Ajuda, 1349-018 Lisboa, Portugal
Madden S.C.:
Service d'Astrophysique, CEA/Saclay, l'Orme des Merisiers, 91191 Gif-sur-Yvette, France
Smith M.W.L.:
Department of Physics and Astronomy, Cardiff University, Parade, Cardiff, CF24 3AA, United Kingdom
Vlahakis C.:
Joint ALMA Office, Alonso de Cordova 3107, Vitacura, Chile
Departamento de Astronomia, Universidad de Chile, Casilla 36-D, Santiago, Chile
Auld R.:
Department of Physics and Astronomy, Cardiff University, Parade, Cardiff, CF24 3AA, United Kingdom
Baes M.:
Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, 9000 Gent, Belgium
De Looze I.:
Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, 9000 Gent, Belgium
Fritz J.:
Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, 9000 Gent, Belgium
Pohlen M.:
Department of Physics and Astronomy, Cardiff University, Parade, Cardiff, CF24 3AA, United Kingdom
Verstappen J.:
Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, 9000 Gent, Belgium
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