Marta Gavilán Bouzas Mercedes Mollá Lorente Estallidos IV, Granada 2-04-07.

Slides:



Advertisements
Similar presentations
A simple model to explain the high gas content of galaxy UGC 8802 Ruixiang Chang Shanghai Astronomical Observatory Collaborators: Jinliang Hou Shiyin Shen.
Advertisements

The extremely high gas content of galaxy UGC8802 Chang Rui-xiang Hou Jin-liang Shen Shi-yin.
Color-magnitude relations of disk galaxies: observations vs. model predictions Ruixiang Chang ( Shanghai Astronomical Observatory ) Collaborators: Jinliang.
T.P. Idiart  and J.A. de Freitas Pacheco   Universidade de São Paulo (Brasil)  Observatoire de la Côte d’Azur (France) Introduction Elliptical galaxies.
STAR-FORMING DWARF GALAXIES: Evolutionary self-consistent models Mariluz Martín-Manjón Mercedes Mollá Ángeles Díaz Roberto Terlevich VII Workshop Estallidos,
Low-metallicity galaxies at low redshifts Y. I. Izotov Main Astronomical Observatory, Kyiv, Ukraine.
 High luminosity from the galactic central region L bol ~ erg/s  High X-ray luminosity  Supermassive black hole at the center of the galaxy.
LOGO The Chemical and Color Evolution of M Reporter: Jun Yin (Shao) Supervisor: Jinliang Hou (Shao)
Early evolution of tidal dwarf galaxies Simone Recchi INAF – Trieste Observatory V Estallidos Workshop “Star Formation and Metallicity” Albayzin – Granada.
RESULTS AND ANALYSIS Mass determination Kauffmann et al. determined masses using SDSS spectra (Hdelta & D4000) Comparison with our determination: Relative.
Looking for the siblings of the Sun Borja Anguiano & RAVE collaboration.
September 6— Starburst 2004 at the Institute of Astronomy, Cambridge Constraints on Lyman continuum flux escaping from galaxies at z~3 using VLT.
Dark Matter and Galaxy Formation Section 4: Semi-Analytic Models of Galaxy Formation Joel R. Primack 2009, eprint arXiv: Presented by: Michael.
The Dwarf Starburst Galaxy NGC 1705 : New H II Region Element Abundances & Reddening Variations Near the Center NGC 1705 is a nearby dwarf starburst galaxy.
Bruno Henriques Claudia Maraston & the Marie Curie Excellence Team Guinevere Kauffmann, Pierluigi Monaco Evolution of the Near-Infrared Emission from Galaxies:
The Complex Star Formation History of NGC 1569 L. Angeretti 1, M. Tosi 2, L. Greggio 3, E. Sabbi 1, A. Aloisi 4, C. Leitherer 4 The object The observations.
Are Galactic Winds Shaping the Properties of Dwarf Galaxies? Konstantinos Tassis The University of Chicago Andrey Kravtsov University of Chicago Nick GnedinFermilab,
The future of astrochemistry of star-forming regions and Hot topics for observers.
Exploring the orbits of the stars from a blind chemical tagging experiment Borja Anguiano Macquarie University, Sydney, Australia.
8th Sino-German Workshop Kunming, Feb 23-28, 2009 Milky Way vs. M31: a Tale of Two Disks Jinliang HOU In collaboration with : Ruixiang CHANG, Shiyin SHEN,
Collaborators : Valentine Wakelam (supervisor)
The Gas Properties of Galaxies on and off of a Star-Forming Sequence David Schiminovich + GALEX Science Team Columbia University.
1 Lessons from cosmic history Star formation laws and their role in galaxy evolution R. Feldmann UC Berkeley see Feldmann 2013, arXiv:
Maxime KUBRYK, IAP, Ph.D student advisors: Nikos PRANTZOS, IAP Lia ATHANASSOULA, OAMP LIA-ORIGINS, May 2012.
After decoupling, overdense regions collapse IF Collapse timefor all sizes. More small ripples than large waves. --> Universe dominated by globular clusters.
1 / 17 The Elemental Abundance Distributions of Milky Way Satellite Galaxies Evan Kirby (HF09) Caltech Small Magellanic Cloud, HST/ACS credit: NASA, ESA,
White Dwarf Binaries in Globular Clusters Fred Rasio (Northwestern)
The coordinated growth of stars, haloes and large-scale structure since z=1 Michael Balogh Department of Physics and Astronomy University of Waterloo.
“Nature and Descendants of Sub-mm and Lyman-break Galaxies in Lambda-CDM” Juan Esteban González Collaborators: Cedric Lacey, Carlton Baugh, Carlos Frenk,
Comprehensive Stellar Population Models and the Disentanglement of Age and Metallicity Effects Guy Worthey 1994, ApJS, 95, 107.
AIMS OF G ALACTIC C HEMICAL E VOLUTION STUDIES To check / constrain our understanding of stellar nucleosynthesis (i.e. stellar yields), either statistically.
Mixing of metals in blue LSB galaxies (or How one can measure their ages) Yuri Shchekinov (Southern Federal U) Eduard Vorobyov (St. Marry U, S Fed U) Domink.
High mass X-ray binaries and recent star formation in the host galaxy P.Shtykovskiy, M.Gilfanov IKI, Moscow; MPA, Garching.
Modeling the dependence of galaxy clustering on stellar mass and SEDs Lan Wang Collaborators: Guinevere Kauffmann (MPA) Cheng Li (MPA/SHAO, USTC) Gabriella.
PI Total time #CoIs, team Fernando Comerón 2n (ELT 42m) Not many people Low-mass brown dwarf formation in the Magellanic Clouds: A population long gone.
Modelling the Stellar Populations of The Milky Way and Andromeda Collaborators: Theory:Observations: Kathryn Johnston (Columbia) Annette Ferguson (Edinburgh)
The dynamics of the gas regulator model and the implied cosmic sSFR-history Yingjie Peng Cambridge Roberto Maiolino, Simon J. Lilly, Alvio Renzini.
野口正史 (東北大学).  Numerical simulation Disk galaxy evolution driven by massive clumps  Analytical model building Hubble sequence.
By Soren S. Larsen (arXiv: ) Reporter: Sun Wei.
Galactic Evolution Workshop NAOJ Sachie Arao, Yuhri Ishimaru (ICU) Shinya Wanajo(Riken) Nucleosynthesis of Elements heavier than Fe through.
Calibración de trazadores de formación estelar mediante modelos de síntesis Héctor Otí-Floranes, J. M. Mas-Hesse & M. Cerviño SEA, Santander, 11 de julio.
Gas Accretion and Secular Processes 1  How much mass assembled in mergers?  How much through gas accretion and secular evolution? Keres et al 2005, Dekel.
What determines the gas content of galaxies?. Galaxy formation - a reminder of the puzzle The fraction of baryons that are “cold” (stars+cold gas) is.
Model Chemical Evolution: Starburst Environment. Once upon a time… Somewhat big bang started it all. Radiation domination Matter domination Matter gets.
Chemical Evolution Models forDwarf Spheroidal Galaxies Gustavo A. Lanfranchi Núcleo de Astrofísica Teórica - Universidade Cruzeiro do Sul Chemical evolution.
Stellar Population Mass Estimates Roelof de Jong (STScI AIP) Eric Bell (MPIA Univ. of Michigan)
Semi-analytical model of galaxy formation Xi Kang Purple Mountain Observatory, CAS.
SPH Simulations of the Galaxy Evolution NAKASATO, Naohito University of Tokyo.
OWLS: OverWhelmingly Large Simulations The formation of galaxies and the evolution of the intergalactic medium.
14-The Evolution of Stars and Gas in Galaxies. Elliptical Galaxies.
Sébastien Muller (ASIAA, Taiwan) M. Guélin (IRAM) M. Dumke (ESO) R. Lucas (IRAM) Probing isotopic ratios at z=0.89 Molecular line absorptions in front.
A comprehensible trace of formation and chemical enrichment of a given stellar system involves the built of several chemical diagrams describing the evolution.
CIfAR Stanford 2008 SN Ia Rates: Theory, Progenitors, and Implications.
Galaxy evolution in z=1 groups The Gemini GEEC2 survey Michael Balogh Department of Physics and Astronomy University of Waterloo.
On the initial conditions and evolution of isolated galaxy models 2012 Workshop on Computational Sciences and Research Hub Induck Hall at Pusan Nat'l University.
Dwarf Irregular Galaxies Models Marta Gavilán Mercedes Mollá Ángeles Díaz NGC 6822 DDO 187.
盘状星系的颜色和颜色梯度 常 瑞 香 (上海天文台 ) 合作者:沈世银 刘成则 侯金良 邵正义 颜色 - 星等关系 颜色梯度 盘状星系的演化模型.
A self consistent model of galaxy formation across cosmic time Bruno Henriques Simon White, Peter Thomas Raul Angulo, Qi Guo, Gerard Lemson, Volker Springel.
Genevieve J. Graves University of California, Santa Cruz
NEW EVOLUTIONARY MODELS OF HII GALAXIES
The Stellar Population of Metal−Poor Galaxies at z~1
GRB : high-z GRBs as a new tool to study the reionization epoch
Mikako Matsuura National Astronomical Observatory of Japan
On the
Modeling the dependence of galaxy clustering on stellar mass and SEDs
Galactic Astronomy 銀河物理学特論 I Lecture 3-4: Chemical evolution of galaxies Seminar: Erb et al. 2006, ApJ, 644, 813 Lecture: 2012/01/23.
Methanol emission from low mass protostars
Authod: Ryan L. Sanders et al.(2018)
Modeling Star Formation and Chemical Evolution in the Local Group dwarfs Oleg Gnedin University of Michigan.
Presentation transcript:

Marta Gavilán Bouzas Mercedes Mollá Lorente Estallidos IV, Granada

What are we looking for? We are looking for some signs to know if dwarf galaxies lose some of their gas or not. How do we looking for it? Our aim is to have a large amount of model results (in an autoconsistent way) to obtain the maximum number of clues. We analized: gas content, metallicity and photometry and compare them with observations.

A short review Galactic Chemical Evolution Model Grid of models

Galactic Chemical Evolution Model The free parameters are: the collapse time: Tcol the efficiency in forming molecular clouds:   the efficiency in transform the clouds into stars:  h The SFR is a RESULT not an INPUT There are no STAR BURSTS: the star forming process is continuous, but not constant

Grid of Models Mass interval: Six values From M  to M  Collapse time: Four values From 8 Gyr to 60 Gyr Star Formation Parameters: Four values S, M, L, XL TOTAL GRID: 96 Models

SFR HISTORIES Lower Tcol and Higher   and  h    Higher Tcol and Lower   and  h    Efficiency=0.88 Efficiency=0.40 Efficiency=0.17

Effective Yield p = The gas fraction estimation

Oxygen Effective Yield f Mgas/fYo Mgas*fYo

Oxygen Abundance Models Garnett 02 DwGx Van Zee 06 Garnett 02 S Ln(1/  ) Tot

IIZw70 Kherig and col 2007  = 0.30  = 0.24  = 0.21  = 0.40

Other observations M(HI) Observations Kong M  Cox et al M  Larsen et al M  Mas-Hesse & Kunth M  Our Model M  < M(HI) < M  M B Observations Kong Gil de Paz et al Cairós et al Cox et al Larsen et al Our Model < M B <-16.7

CONCLUSIONS Our models present an effective yield without gas outflow according with most observations. The models with high efficiency give too much high abundances. It is possible that they do not match with any observations. In the case of IIZw70 we reproduce the SFR and the (O/H) value with no star burst. …but the gas content needs additional explanation.