SIMPLE-FEEDBACK · Fedback in low mass galaxies at z>1 : a SIMPLE study
7РП — „Хора“ (Действия „Мария Кюри“)
- Период
- 2009-10-01 → 2012-01-31
- Финансиране от ЕС
- 334 095 €
- Участници
- 1
- Схема
- MC-IOF
Линиите свързват координатора с партньорите.
Накратко на български
Галактическите ветрове в малки галактики далеч в Космоса се анализират чрез спектрове на квазари и телескопи. Това помага да се разбере защо формирането на галактики е неефективно и как се регулира количеството газ в тях.
Кратко обяснение, генерирано от езиков модел по текста на CORDIS. Оригиналът е по-долу.
Резултати накратко
Fedback in low mass galaxies at z>1 : a SIMPLE study
Project aims and objectives Galaxy formation is very inefficient. On average, only 5 % of baryons made it in galaxies. 'Why is galaxy formation so inefficient?' is one of the most fundamental questions in modern astrophysics. This question is directly related to the mechanisms that regulate gas supply/gas losses. A large number of observations have shown that galactic outflows are important in regulating the gas content of galaxies. However, in spite of rapid progress, our current knowledge of the physical properties of galactic winds is still in its infancy. Little is known on the mass outflow rate, for instance. The main goal of this project is to understand the physical properties of galactic winds produced by star-forming galaxies and how they might depend on the galaxy properties (such as mass, star-formation rate, etc.). In order to achieve our main objective, we have selected a dozen low-mass galaxies 'caught in the act' of producing super-winds half way across the universe (at redshift z = 1) where the wind signature is seen in background quasar spectra. For each of these galaxies, we have obtained detailed 2-dimensional kinematics with the SINFONI instrument of one of the Very Large Telescopes (VLT) of the European Southern Observatory (ESO). For each of the quasars, we also have detailed absorption kinematics along the Quasi-stellar object (QSO) line-of-sight, also obtained at the European Southern Observatory. The objectives planned for this project were to exploit the available data in order to (i) assess the dynamical state of the starbursts, and (ii) extract the physical properties of the intervening gas. We have analysed the data, computed the star-formation rates, the dynamical masses of the galaxies from the SINFONI maps. Another key aspect of our project is to understand the absorption kinematics in the context of galactic winds and we recently successfully achieved this milestone. For this, we needed to model the galactic outflow. Using a simple bi-conical flow, we could demonstrate that the absorption kinematics seen in the quasar spectra could be very well accounted for.
Текст от CORDIS, на английски · Данни: CORDIS, © Европейски съюз
Цел на проекта
Current observations and models indicate that supernova feedback processes are important in shaping many properties of galaxies. In spite of rapid progress, our current knowledge of the physical properties of super-winds is still in its infancy: it comes mainly from few nearby galaxies or from bright ultra-luminous infra-red galaxies where the kinematics of the winds are inferred from the blue-shifted sodium absorption of the cold entrained gas against the galaxy continuum, i.e. along radial sight lines. We are studying low-mass galaxies caught in the act" of producing super-winds half-way across the universe (at z=1) using the MgII resonance line in QSO spectra. A unique aspect of our project is that we are combining the 2D spatially-resolved kinematics of starbursts with the 1D kinematics of the absorbing gas seen along the quasar sight line. Our scientific goals, however, extend much beyond our sample. While at the outgoing host, the University of California, Santa Barbara (UCSB), working with Prof. C. Martin, we aim to combine our results on intervening sight-lines with upcoming surveys on radial sight-lines in order to put both in a unified context. This will give us constraints on the radial properties of outflows. In addition, given that our sample nicely fills unexplored mass and SFR ranges, we will quantify how the wind properties vary over a much wider range of masses and star-formation rates. At the returning host, the Laboratoire Astrophysique de Toulouse-Tarbes (LATT), the fellow will prepare, design and exploit the next-generation of feedback surveys using the wide field integral field unit, MUSE, which will provide unprecedented 3-dimensional data sets on thousands of faint emission line galaxies, and spectra of hundreds of galaxy-galaxy and galaxy-quasar pairs. In other words, the skills acquired at the outgoing host will be very valuable to exploit the MUSE instrument, which is one major training objective."
Оригинален текст от CORDIS (на английски).
Участници
- UNIVERSITE PAUL SABATIER TOULOUSE III · Toulouse Cedex 9КоординаторФранция
Връзки
Данни: CORDIS, © Европейски съюз