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Your search keyword '"galaxies ISM"' showing total 2 results
Start Over Descriptor "galaxies ISM" Topic astrophysics - cosmology and nongalactic astrophysics
2 results on '"galaxies ISM"'

1. Impact of H2-driven star formation and stellar feedback from low-enrichment environments on the formation of spiral galaxies

Author

Milena Valentini, Klaus Dolag, Stefano Borgani, Giuseppe Murante, Umberto Maio, Luca Tornatore, Gian Luigi Granato, Cinthia Ragone-Figueroa, Andreas Burkert, Antonio Ragagnin, Elena Rasia, Valentini, Milena, Dolag, Klau, Borgani, Stefano, Murante, Giuseppe, Maio, Umberto, Tornatore, Luca, Granato, Gian Luigi, Ragone-Figueroa, Cinthia, Burkert, Andrea, Ragagnin, Antonio, and Rasia, Elena

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies spiral, FOS: Physical sciences, Astronomy and Astrophysics, galaxies ISM, Astrophysics - Astrophysics of Galaxies, galaxies evolution, galaxies formation, Astrophysic, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies stellar content, Astrophysics of Galaxie, methods numerical, Cosmology and Nongalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The reservoir of molecular gas (H$_{\rm 2}$) represents the fuel for the star formation (SF) of a galaxy. Connecting the star formation rate (SFR) to the available H$_{\rm 2}$ is key to accurately model SF in cosmological simulations of galaxy formation. We investigate how modifying the underlying modelling of H$_{\rm 2}$ and the description of stellar feedback in low-metallicity environments (LMF, i.e. low-metallicity stellar feedback) in cosmological, zoomed-in simulations of a Milky Way-size halo influences the formation history of the forming, spiral galaxy and its final properties. We exploit two different models to compute the molecular fraction of cold gas (f$_{\rm H_{\rm 2}}$): $i)$ the theoretical model by Krumholz et al. (2009b) and $ii)$ the phenomenological prescription by Blitz & Rosolowsky (2006). We find that the model adopted to estimate f$_{\rm H_{\rm 2}}$ plays a key role in determining final properties and in shaping the morphology of the galaxy. The clumpier interstellar medium (ISM) and the more complex H$_{\rm 2}$ distribution that the Krumholz et al. (2009b) model predicts result in better agreement with observations of nearby disc galaxies. This shows how crucial it is to link the SFR to the physical properties of the star-forming, molecular ISM. The additional source of energy that LMF supplies in a metal-poor ISM is key in controlling SF at high redshift and in regulating the reservoir of SF across cosmic time. Not only is LMF able to regulate cooling properties of the ISM, but it also reduces the stellar mass of the galaxy bulge. These findings can foster the improvement of the numerical modelling of SF in cosmological simulations., accepted for publication in MNRAS

Published
2022
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2. The Herschel Virgo Cluster Survey - XII. FIR properties of optically selected Virgo cluster galaxies

Author

S. Alighieri di Serego, George J. Bendo, S. C. Madden, Stefano Zibetti, Catherine Vlahakis, Dominik J. Bomans, Médéric Boquien, Alessandro Boselli, I. De Looze, L. K. Hunt, Joris Verstappen, Laure Ciesla, Maarten Baes, Michael Pohlen, Laura Magrini, Giuseppe Gavazzi, M. S. Clemens, Marco Grossi, Jacopo Fritz, Matthew Smith, Robbie Richard Auld, Simone Bianchi, E. M. Xilouris, Ciro Pappalardo, Edvige Corbelli, Luca Cortese, Jonathan Ivor Davies, AUTRES, Space Telescope European Coordinating Facility (STECF), Space Telescope European Coordinating Facility, European Southern Observatory (ESO), Universiteit Gent = Ghent University (UGENT), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Biophotonique et Pharmacologie - UMR 7213 (LBP), Centre National de la Recherche Scientifique (CNRS)-Réseau nanophotonique et optique, Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB), Centro de Astronomia e Astrofísica da Universidade de Lisboa (CAAUL), Universidade de Lisboa = University of Lisbon (ULISBOA), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), School of Physics and Astronomy [Cardiff], Cardiff University, Sterrenkundig Observatorium, Universiteit Gent = Ghent University [Belgium] (UGENT), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB), Universidade de Lisboa (ULISBOA), Universiteit Gent, Universiteit Gent [Ghent], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Universitá degli Studi di Milano-Bicocca, Universitá degli Studi di Milan-Bocca, Auld, R, Bianchi, S, Smith, M, Davies, J, Bendo, G, di Serego Alighieri, S, Cortese, L, Baes, M, Bomans, D, Boquien, M, Boselli, A, Ciesla, L, Clemens, M, Corbelli, E, De Looze, I, Fritz, J, Gavazzi, G, Pappalardo, C, Grossi, M, Hunt, L, Madden, S, Magrini, L, Pohlen, M, Verstappen, J, Vlahakis, C, Xilouris, E, and Zibetti, S

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), DWARF GALAXIES, Population, Extinction (astronomy), MU-M, FOS: Physical sciences, Astrophysics, 01 natural sciences, galaxies [infrared], MAGELLANIC CLOUDS, 0103 physical sciences, NEARBY GALAXIES, COLD DUST, education, 010303 astronomy & astrophysics, QB, Dwarf galaxy, clusters of galaxies galaxy Virgo, Physics, Luminous infrared galaxy, education.field_of_study, Spiral galaxy, II. DUST, ISM [galaxies], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, extinction, infrared galaxies, Astronomy, Astronomy and Astrophysics, clusters: individual: Virgo [galaxies], galaxies ISM, Virgo Cluster, Galaxy, GAS MASS-RATIO, Physics and Astronomy, Space and Planetary Science, Elliptical galaxy, photometry [galaxies], dust, extinction, dust, SUBMILLIMETER, galaxies photometry, SCIENCE DEMONSTRATION PHASE, SPIRAL GALAXIES, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Herschel Virgo Cluster Survey (HeViCS) is the deepest, confusion-limited survey of the Virgo Cluster at far-infrared (FIR) wavelengths. The entire survey at full depth covers $\sim$55 sq. deg. in 5 bands (100-500 \micron), encompassing the areas around the central dominant elliptical galaxies (M87, M86 & M49) and extends as far as the NW cloud, the W cloud and the Southern extension. The survey extends beyond this region with lower sensitivity so that the total area covered is 84 sq. deg. In this paper we describe the data, the data acquisition techniques and present the detection rates of the optically selected Virgo Cluster Catalogue (VCC). We detect 254 (34%) of 750 VCC galaxies found within the survey boundary in at least one band and 171 galaxies are detected in all five bands. For the remainder of the galaxies we have measured strict upper limits for their FIR emission. The population of detected galaxies contains early- as well as late-types although the latter dominate the detection statistics. We have modelled 168 galaxies, showing no evidence of a strong synchrotron component in their FIR spectra, using a single-temperature modified blackbody spectrum with a fixed emissivity index ($\beta = 2$). A study of the $\chi^2$ distribution indicates that this model is not appropriate in all cases, and this is supported by the FIR colours which indicate a spread in $\beta$=1--2. Statistical comparison of the dust mass and temperature distributions from 140 galaxies with $\chi^2_{dof=3} < 7.8$ (95% confidence level) shows that late-types have typically colder, more massive dust reservoirs; the early-type dust masses have a mean of ${\rm log}( / M_{\sun}) = 6.3 \pm 0.3 $, while for late-types ${\rm log}( / M_{\sun}) =7.1 \pm 0.1$... (abridged), Comment: 47 pages, 14 figures, 6 tables, accepted for publication in MNRAS

Published
2013
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