PASTIS: Probing Abundances and Star formation Timescales with Integral field Spectroscopy Anna Gallazzi INAF - Osservatorio Astrofisico di Arcetri
|
|
- Lisa Robertson
- 5 years ago
- Views:
Transcription
1 Co- funded by the European Union PASTIS: Probing Abundances and Star formation Timescales with Integral field Spectroscopy Anna Gallazzi INAF - Osservatorio Astrofisico di Arcetri Stefano Zibetti, Filippo Mannucci (INAF-OAA), Eric Bell (Michigan), Jarle Brinchmann (Leiden), Sune Toft, Andrew Zirm (DARK), Anna Pasquali (ARI-Heidelberg), Jakob Walcher (AIP), Paula Coelho (Sao Paulo), Stephane Charlot (IAP) CALIFA collaboration LVII Congresso SAIt, 9/5/2013
2 THE IDEA BEHIND PASTIS Age and chemical composition of stars and ISM main epoch of SF, its duration and efficiency Dynamical mass and structure SF and assembly histories Linking age and chemical properties with galaxy mass and structure can provide important clues to how SF and mass assembly relate to each other Different measures of chemical enrichment in relation to age, star formation and structural properties both on local and global scales Constraining typical timescales of star formation and chemical enrichment in relation to galaxy structure and environment Archaeological versus direct approach: Is the inferred timescale consistent with observed evolution of galaxy scaling relations?
3 HOW CAN WE STUDY THEM? OBSERVATIONAL CONSTRAINTS Physical parameters of unresolved stellar populations are encoded in integrated galaxy spectra Individual absorption features are almost insensitive to dust attenuation and help in breaking age-metallicity degeneracy [Lick system; e.g. Worthey+94, Trager+2000, Sanchez-Balzquez +06..G05] full spectrum fitting [MOPED, VESPA, Starlight, STECKMAP, PCA analysis Ferreras+06, see Walcher +10 review] H Balmer absorption [Z/H] H Balmer absorption Older Bursts of [Mg2Fe] ~ metallicity 4000A -break
4 A BAYESIAN APPROACH MONTE CARLO LIBRARY OF COMPLEX SFH AND METALLICITIES: exponential SFH + random burst; metallicity fixed for each model (i.e. no chemical evolution) - based on BC03 convolve models to galaxy velocity dispersion and measure absorption index strengths as in observed spectra build full probability density function of STELLAR MASS, LUMINOSITY- AND MASS-WEIGHTED AGE, STELLAR METALLICITY Optimal set of absorption features: D4000, Hβ, Hγ+Hδ, [Mg 2 Fe], [MgFe] Age Metallicity
5 GALAXY SCALING RELATIONS Chemical enrichment Stellar Age [ /Fe] abundance ratio M * ~ 3x10 10 Stellar mass Gallazzi et al 2005 THOMAS ET AL 2010 Gas metallicity Mannucci et al 2010 Large spectroscopic surveys have provided a quantitative description of present-day galaxy populations Mass is the primary parameter in determining the age and metallicity of present-day galaxies Scatter depends on galaxy morphology and on star formation activity Analogy between metallicity of stars and metallicity of gas in star-forming galaxies
6 THE REDSHIFT EVOLUTION OF STELLAR POPULATIONS Still limited knowledge about the evolution with redshift of the stellar populations in galaxies Deep multi-object spectroscopy with IMACS on Magellan for a sample of 80 galaxies selected at 0.65<z<0.75 Well-defined red-sequence of quiescent galaxies at z=0.7 with similar metallicities as present-day galaxies and ages consistent with oldest present-day galaxies, under passive evolution Population of intermediate-mass star-forming galaxies at z=0.7 could contribute to the younger and more metal-rich fraction of local massive galaxies Residuals in age and metallicity correlate with specific SFR NIR multi-object spectrographs will allow to extend evolutionary studies out to z 2 (only a handful of objects so far) Gallazzi et al, 2013, to be subm.
7 IMPROVING THE FOSSIL RECORD Robust estimates of α/fe for galaxies with different star formation activity Updated Coelho et al 2007 and Walcher et al 2009 differential SPS models with variable α/fe and Fe/H at high spectral resolution and down to few-tens-myr populations Most spectra of low-redshift galaxies lack spatially resolved information: prevent studying correlated spatial variations in stellar populations, gas and kinematic properties, which are the record of galaxy assembly history incomplete and unresolved coverage can translate into severe biases in derived physical properties: affect comparison with galaxy formation models and assessment of redshift evolution CALIFA: the Calar Alto Legacy Integral Field Area survey (PI: S.Sanchez)
8 Courtesy Sebastian Sanchez Sanchez et al 2012 Husemann et al 2013 Color CALIFA survey at the 3.5m CAHA telescope with PMAS/PPAK IFU 600 diameter-selected low-redshift (z<0.03) galaxies spanning the whole color magnitude space Magnitude high and low spectral resolution set-up covering the whole optical range ( A ) ideal for emission line and absorption/stellar continuum studies DR1 of 100 objects:
9 gas velocity field emission lines THE MICE major merger of two massive gas-rich galaxies after first passage star formation stellar populations Wild et al 2013, submitted
10 NGC e11M NGC0776 5e10M NGC0001 4e10M
11 NGC e11M NGC0776 5e10M NGC0001 4e10M
12 WORK IN PROGRESS... Stellar population gradients as a function of mass and morphology derive un-biased galaxy scaling relations stellar metallicity Stellar and gas-phase metallicities trace different phases of chemical evolution. How do they correlated on local scales? How is the scatter correlated with age and α/fe (SF timescale)? Gain insight into the synchronization of the enrichment of the two phases and the occurrence of inflows/outflows at certain stages of galaxy evolution Stellar mass Gallazzi et al 2005 gas-phase metallicity Dynamical (total) versus stellar mass: link between SF and assembly processes Confirm and better quantify the age dependence of the DM fraction and explore any correlation of SF timescale Gallazzi et al 2006 Dynamical (total) mass
Element abundance ratios and star formation quenching: satellite versus central galaxies
Element abundance ratios and star formation quenching: satellite versus central galaxies Anna Gallazzi INAF-Osservatorio Astrofisico di Arcetri Co#funded)by)the)) European)Union) with: Anna Pasquali (ARI-Heidelberg)
More informationCALAR ALTO LEGACY INTEGRAL FIELD AREA SURVEY OVERVIEW, STATUS & LATEST RESULTS
CALAR ALTO LEGACY INTEGRAL FIELD AREA SURVEY OVERVIEW, STATUS & LATEST RESULTS Jesús Falcón-Barroso www.iac.es/project/traces THE CALIFA TEAM THE CALIFA SURVEY www.caha.es/califa IFU survey using the PPAK@3.5m
More informationLEGA-C. The Physics of Galaxies 7 Gyr Ago. Arjen van der Wel Max Planck Institute for Astronomy, Heidelberg
LEGA-C The Physics of Galaxies 7 Gyr Ago Arjen van der Wel Max Planck Institute for Astronomy, Heidelberg How do galaxies assemble their stellar bodies? Collection of large samples at large lookback times
More informationThe Stellar Populations of Galaxies H. W. Rix IMPRS Galaxies Course March 11, 2011
The Stellar Populations of Galaxies H. W. Rix IMPRS Galaxies Course March 11, 2011 Goal: Determine n * (M *,t age,[fe/h],r) for a population of galaxies How many stars of what mass and metallicity formed
More informationarxiv: v1 [astro-ph.co] 2 Dec 2011
The Spectral Energy Distribution of Galaxies Proceedings IAU Symposium No. 284, 2011 R.J. Tuffs & C.C.Popescu, eds. c 2011 International Astronomical Union DOI: 00.0000/X000000000000000X Spectral models
More informationYicheng Guo (UCO/Lick, UCSC)
Formation and Evolution of Clumpy Galaxies at z=0.5--3 Yicheng Guo (UCO/Lick, UCSC) Collaborators: Henry Ferguson, Eric Bell, David Koo, Chris Conselice, Mauro Giavalisco, Nir Mandelker, Swara Ravindranatch,
More informationStePs. Angela Iovino INAF OABrera On behalf of the StePs team*
StePs Stellar Populations at intermediate redshift survey Angela Iovino INAF OABrera On behalf of the StePs team* * B. Poggianti, A. Iovino, A. Mercurio, L. Pozzetti, A. Gallazzi, M. Bolzonella, S. Zibetti,
More informationStar Formation Indicators
Star Formation Indicators Calzetti 2007 astro-ph/0707.0467 Brinchmann et al. 2004 MNRAS 351, 1151 SFR indicators in general! SFR indicators are defined from the X ray to the radio! All probe the MASSIVE
More informationThe star formation history of Virgo spiral galaxies
The star formation history of Virgo spiral galaxies Combined spectral and photometric inversion Ciro Pappalardo INAF Osservatorio Astrofisico di Arcetri Cluster galaxies Abell 1689 Physical effects acting
More informationChapter 10: Unresolved Stellar Populations
Chapter 10: Unresolved Stellar Populations We now consider the case when individual stars are not resolved. So we need to use photometric and spectroscopic observations of integrated magnitudes, colors
More informationPyParadise. Developed by: Bernd Husemann (MPIA), Omar Choudhury (AIP)! C. Jakob Walcher Leibniz Institut für Astrophysik Potsdam (AIP)
PyParadise Developed by: Bernd Husemann (MPIA), Omar Choudhury (AIP)! C. Jakob Walcher Leibniz Institut für Astrophysik Potsdam (AIP) Physical properties Physics 101: A physical property is described by
More informationDeriving stellar masses from SDSS
Deriving stellar masses from SDSS Reference: Bruzual and Charlot 2003MNRAS.344.1000B Kauffmann et al. 2003MNRAS.341.33 Salim et al. 2007ApJS..173..267S Bell et al. 2003ApJS..149..289B Outline! Basic idea!
More informationAstr 5465 Feb. 13, 2018 Distribution & Classification of Galaxies Distribution of Galaxies
Astr 5465 Feb. 13, 2018 Distribution & Classification of Galaxies Distribution of Galaxies Faintest galaxies are distributed ~ uniformly over the sky except for the Galactic plane (zone of avoidance) Brighter
More informationThe ALMA z=4 Survey (AR4S)
The ALMA z=4 Survey (AR4S) ALMA studies of massive z~4-5 galaxies Corentin Schreiber Leiden University October 21 2016 In collaboration with: Maurilio Pannella, David Elbaz, Roger Leiton, Tao Wang, and
More informationMeasuring star formation in galaxies and its evolution. Andrew Hopkins Australian Astronomical Observatory
Measuring star formation in galaxies and its evolution Andrew Hopkins Australian Astronomical Observatory Evolution of Star Formation Evolution of Star Formation Evolution of Star Formation Evolution of
More informationBUILDING GALAXIES. Question 1: When and where did the stars form?
BUILDING GALAXIES The unprecedented accuracy of recent observations of the power spectrum of the cosmic microwave background leaves little doubt that the universe formed in a hot big bang, later cooling
More informationVivienne Wild. Timing the starburst AGN connection
Vivienne Wild Timing the starburst AGN connection There are many theories successful in explaining the observed correlations between black holes and their host galaxies. In turn, these theories play a
More informationStellar populations model predictions in the UV spectral range
INSTITUTO DE ASTROFÍSICA DE CANARIAS Alexandre Vazdekis M. Koleva, E. Ricciardelli, Falcón-Barroso Stellar populations model predictions in the UV spectral range The UV spectral range The youngest stellar
More informationarxiv: v1 [astro-ph.ga] 20 Mar 2012
Bull. Astr. Soc. India (2011) 00, 1 8 arxiv:1203.4304v1 [astro-ph.ga] 20 Mar 2012 Modelling chemical abundance anticorrelations on globular cluster spectra P. Coelho 1, S. Percival 2 and M. Salaris 2 1
More informationDeep Keck Spectroscopy of High-Redshift Quiescent Galaxies
Sirio Belli Max-Planck Institute for Extraterrestrial Physics Deep Keck Spectroscopy of High-Redshift Quiescent Galaxies with Andrew Newman and Richard Ellis Introduction Schawinski et al. 2014 red sequence
More informationStudying stars in M31 GCs using NIRI and GNIRS
Studying stars in M31 GCs using NIRI and GNIRS Ricardo Schiavon Gemini Observatory GSM 2012 San Francisco July 19, 2012 Collaborators Andy Stephens (Gemini) Nelson Caldwell (SAO) Matthew Shetrone (HET)
More informationDust [12.1] Star clusters. Absorb and scatter light Effect strongest in blue, less in red, zero in radio.
More abs. Dust [1.1] kev V Wavelength Optical Infra-red More abs. Wilms et al. 000, ApJ, 54, 914 No grains Grains from http://www.astro.princeton.edu/~draine/dust/dustmix.html See DraineH 003a, column
More informationTwo Main Techniques. I: Star-forming Galaxies
p.1/24 The high redshift universe has been opened up to direct observation in the last few years, but most emphasis has been placed on finding the progenitors of today s massive ellipticals. p.2/24 Two
More informationIMF variations in unresolved stellar populations: Challenges
Department of Space and Climate Physics Mullard Space Science Laboratory http://www.ucl.ac.uk/mssl IMF variations in unresolved stellar populations: Challenges Ignacio Ferreras Mullard Space Science Laboratory
More informationFollowing the evolution of the Galactic disc with Open Clusters
Following the evolution of the Galactic disc with Open Clusters Laura Magrini INAF-Osservatorio Astrofisico di Arcetri With Nikos Prantzos and the GES collaboration (in particular Lorenzo Spina, Sofia
More informationStellar Population Mass Estimates. Roelof de Jong (STScI AIP) Eric Bell (MPIA Univ. of Michigan)
Stellar Population Mass Estimates Roelof de Jong (STScI AIP) Eric Bell (MPIA Univ. of Michigan) Overview Stellar Mass-to-Light (M/L) ratios from SEDs Comparing different SED fitting techniques Comparing
More informationThe LEGA-C Survey: The Physics of Galaxies 7 Gyr Ago
The LEGA-C Survey: The Physics of Galaxies 7 Gyr Ago Arjen van der Wel Kai Noeske Rachel Bezanson Camilla Pacifici 3 Anna Gallazzi Marijn Franx Juan-Carlos Muñoz-Mateos Eric F. Bell 7 Gabriel Brammer 8
More informationSpectral Energy Distribution of galaxies
Spectral Energy Distribution of galaxies Paola Santini PhD in Astronomy, Astrophysics and Space Science A.A. 2013 2014 Key points lecture 1 Multiwavalength astronomy: 1. Gives a complete view of the galaxy
More informationThe The largest assembly ESO high-redshift. Lidia Tasca & VUDS collaboration
The The largest assembly ESO high-redshift of massive Large galaxies Programme at 2
More informationRest-frame Optical Spectra: A Window into Galaxy Formation at z~2
Rest-frame Optical Spectra: A Window into Galaxy Formation at z~2 Alice Shapley (UCLA) Collaborators: Mariska Kriek, Naveen Reddy, Brian Siana, Alison Coil, Bahram Mobasher, Bill Freeman, Ryan Sanders,
More informationSpectroscopy of M81 Globular Clusters. Julie B. Nantais & John P. Huchra MMT Science Symposium 5/19/10
Spectroscopy of M81 Globular Clusters Julie B. Nantais & John P. Huchra MMT Science Symposium 5/19/10 Galaxy Formation and Globular Clusters Questions: How did galaxies get to be different? Did all galaxies
More informationThe needs and desires of stellar population models. Scott Trager
The needs and desires of stellar population models Scott Trager The needs and desires of stellar population model users Scott Trager Desires/motivation We want to know the star formation histories of galaxies
More informationUsing Globular Clusters to. Study Elliptical Galaxies. The View Isn t Bad... Omega Centauri. Terry Bridges Australian Gemini Office M13
Using Globular Clusters to Omega Centauri Study Elliptical Galaxies Terry Bridges Australian Gemini Office 10,000 1,000,000 stars up to 1000 stars/pc3 typical sizes ~10 parsec Mike Beasley (IAC, Tenerife)
More informationThe Star Clusters of the Magellanic Clouds
The Dance of Stars MODEST-14 The Star Clusters of the Magellanic Clouds Eva K. Grebel Astronomisches Rechen-Institut Zentrum für Astronomie der Universität Heidelberg Star Clusters in the Magellanic Clouds!
More informationThe role of cold gas in the chemical evolution of nearby galaxies
The Role of Hydrogen in the Evolution of Galaxies Kuching, 17 th September 2014 The role of cold gas in the chemical evolution of nearby galaxies Tom Hughes Luca Cortese (Swinburne), Alessandro Boselli
More information3D spectroscopy of massive stars, SNe, and other point sources in crowded fields
3D spectroscopy of massive stars, SNe, and other point sources in crowded fields Martin M. Roth Sebastian Kamann, Christer Sandin, Ana Monreal, Peter Weilbacher, Lutz Wisotzki Leibniz-Institut für Astrophysik
More informationarxiv:astro-ph/ v1 15 Jan 2007
**FULL TITLE** ASP Conference Series, Vol. **VOLUME**, **YEAR OF PUBLICATION** **NAMES OF EDITORS** Reconstructing Star Formation Histories of Galaxies Uta Fritze 1 & Thomas Lilly 2 1 University of Hertfordshire,
More informationIntroduction and Motivation
1 Introduction and Motivation This last two days at this conference, we ve focused on two large questions regarding the role that AGNs play in galaxy evolution: My research focuses on exploring these questions
More informationSALT s Venture into Near Infrared Astronomy with RSS NIR
SALT s Venture into Near Infrared Astronomy with RSS NIR Marsha Wolf University of Wisconsin Madison IUCAA RSS VIS future RSS NIR 5 June 2015 SALT Science Conference 2015 2 Robert Stobie Spectrograph 5
More informationStellar populations in the cd galaxy NGC 3311
Stellar populations in the cd galaxy NGC 3311 C. E. Barbosa 1,2, C. Mendes de Oliveira 1, M. Arnaboldi 2, M. Hilker 2, L. Coccato 2, T. Richtler 3 1 Universidade de São Paulo, São Paulo, Brazil 2 European
More informationQuantifying the Assembly History of Elliptical Galaxies
Quantifying the Assembly History of Elliptical Galaxies Michael Pierce (University of Wyoming) A Science Use Case for GMT and TMT Origin of Elliptical Galaxies! Elliptical Galaxies Form Through Mergers!
More informationStellar Population Synthesis: The Role of Adaptive Optics
Stellar Population Synthesis: The Role of Adaptive Optics Jason Melbourne (Caltech) Nearby (2.5 Mpc) Dwarf Irregular Galaxy KKH 98 HST F475W (Blue), HST F814W (Green), Keck AO K-band (red) Melbourne et
More informationObservations of galaxy evolution. Pieter van Dokkum
Observations of galaxy evolution Pieter van Dokkum Overview Broad topic! Split in three conceptually-different parts: ç ç low redshift high redshift 1. Census: what is out there? N (z, L, Mstars, Mdark,
More informationAn analogy. "Galaxies" can be compared to "cities" What would you like to know about cities? What would you need to be able to answer these questions?
An analogy "Galaxies" can be compared to "cities" What would you like to know about cities? how does your own city look like? how big is it? what is its population? history? how did it develop? how does
More informationResolved Star Formation Surface Density and Stellar Mass Density of Galaxies in the Local Universe. Abstract
Resolved Star Formation Surface Density and Stellar Mass Density of Galaxies in the Local Universe Abdurrouf Astronomical Institute of Tohoku University Abstract In order to understand how the stellar
More informationMapping the oxygen abundance in an elliptical galaxy (NGC 5128)
Mapping the oxygen abundance in an elliptical galaxy (NGC 5128) Jeremy R. Walsh, ESO Collaborators: George H. Jacoby, GMT Observatory, Carnegie; Reynier Peletier, Kapteyn Lab., Groningen; Nicholas A. Walton,
More informationSource plane reconstruction of the giant gravitational arc in Abell 2667: a condidate Wolf-Rayet galaxy at z 1
Source plane reconstruction of the giant gravitational arc in Abell 2667: a condidate Wolf-Rayet galaxy at z 1 Speaker: Shuo Cao Department of Astronomy Beijing Normal University Collaborators: Giovanni
More informationWhat do we need to know about galaxy formation?
What do we need to know about galaxy formation? rachel somerville University of Michigan Hubble Science Legacy Workshop April 2002 what s next? test the CDM paradigm constrain the nature of the dark matter
More informationThe Swift GRB Host Galaxy Legacy Survey
The Swift GRB Host Galaxy Legacy Survey (Caltech) + the SHOALS collaboration: Antonio de Ugarte Postigo (IAA) Steve Schulze (PUC) Thomas Kruehler (ESO) Tanmoy Laskar (Harvard) Antonino Cucchiara (GSFC)
More informationBULGES NGC 4710 NGC 4594 ESO 498-G5 NGC 4565 NGC 7457 ESO 1129
BULGES NGC 4594 ESO 498-G5 NGC 4710 ESO 1129 NGC 7457 NGC 4565 FORMATION AND EVOLUTION OF BULGES Classical bulge Presents in early type galaxies: lenticular, Sa Very similar to elliptical : Mg2 - ; Dn
More information13.1 Galaxy Evolution: Introduction
13.1 Galaxy Evolution: Introduction Galaxies Must Evolve Stars evolve: they are born from ISM, evolve, shed envelopes or explode, enriching the ISM, more stars are born Structure evolves: density fluctuations
More informationThe star formation history of mass-selected galaxies in the COSMOS field
IR Emission, ISM and Star Formation, MPIA, Heidelberg February 22 nd 2010 The star formation history of mass-selected galaxies in the COSMOS field The IR-radio relation as a key to understanding galaxy
More informationBursty stellar populations and AGN in bulges
Bursty stellar populations and AGN in bulges Vivienne Wild (MPA Garching, MAGPOP) Guinevere Kauffmann, Tim Heckman Mergers and BH growth: Theory/Simulations Di Matteo, Springel, Hernquist, Nature 2005
More informationAstronomy 330 Lecture Dec 2010
Astronomy 330 Lecture 26 10 Dec 2010 Outline Clusters Evolution of cluster populations The state of HI sensitivity Large Scale Structure Cluster Evolution Why might we expect it? What does density determine?
More informationThe Galaxy Evolution Explorer. Michael Rich, UCLA. Samir Salim Ryan Mallery
The Galaxy Evolution Explorer Michael Rich, UCLA Samir Salim Ryan Mallery A decade long effort: From early proposals for UV imaging telescopes by C. Martin, and the FOCA balloon-borne telescope at LAS
More informationLyα-Emitting Galaxies at z=3.1: L* Progenitors Experiencing Rapid Star Formation
Lyα-Emitting Galaxies at z=3.1: L* Progenitors Experiencing Rapid Star Formation Gawiser et al., 2007 Presented on October 22, 2009 PHYS 689: Galaxy Formation Lyman-α Emitters (LAEs) Lyα line is easily
More informationObserving the Formation of Dense Stellar Nuclei at Low and High Redshift (?) Roderik Overzier Max-Planck-Institute for Astrophysics
Observing the Formation of Dense Stellar Nuclei at Low and High Redshift (?) Roderik Overzier Max-Planck-Institute for Astrophysics with: Tim Heckman (JHU) GALEX Science Team (PI: Chris Martin), Lee Armus,
More informationGalaxies 626. Lecture 9 Metals (2) and the history of star formation from optical/uv observations
Galaxies 626 Lecture 9 Metals (2) and the history of star formation from optical/uv observations Measuring metals at high redshift Metals at 6 How can we measure the ultra high z star formation? One robust
More informationThe evolution of the Galaxy Stellar Mass Function:
The evolution of the Galaxy Stellar Mass Function: towards the high-mass end at high redshifts Helena Domínguez Sánchez Jordi Cepa (IAC), Miguel Sánchez Portal (ESAC), Andrea Cimatti (UniBo), Francesca
More informationIntroduction The interplay between local and global processes in galaxies. C. Jakob Walcher Leibniz Institut für Astrophysik Potsdam (AIP)
Introduction The interplay between local and global processes in galaxies C. Jakob Walcher Leibniz Institut für Astrophysik Potsdam (AIP) Introduction Why this is NOT and IFU conference!! C. Jakob Walcher
More informationarxiv: v1 [astro-ph.ga] 27 Mar 2015
Stellar populations of bulges at low redshift Patricia Sánchez-Blázquez arxiv:1503.08105v1 [astro-ph.ga] 27 Mar 2015 Abstract This chapter summarizes our current understanding of the stellar population
More informationAge Dating A SSP. Quick quiz: please write down a 3 sentence explanation of why these plots look like they do.
Color is only a weak function of age after ~3Gyrs (for a given metallicity) (See MBW pg 473) But there is a strong change in M/L V and weak change in M/L K Age Dating A SSP Quick quiz: please write down
More informationThe relic galaxy NGC 1277
The relic galaxy NGC 1277 EMIR-RIA E.Eftekhari M.Beasley A.Vazdekis M.Balcells F. La Barbera I. Martín Navarro Cádiz, 23-24/11/17 Stellar populations of ETGs as seen from the optical range: CMR of Coma
More informationStar Formation. Spitzer Key Contributions to Date
Star Formation Answering Fundamental Questions During the Spitzer Warm Mission Phase Lori Allen CfA John Carpenter, Caltech Lee Hartmann, University of Michigan Michael Liu, University of Hawaii Tom Megeath,
More informationGalaxies. Need a (physically) meaningful way of describing the relevant properties of a galaxy.
Galaxies Aim to understand the characteristics of galaxies, how they have evolved in time, and how they depend on environment (location in space), size, mass, etc. Need a (physically) meaningful way of
More informationM31 Color Mag Diagram Brown et al 592:L17-L20!
The physical origin of the form of the IMF is not well understood Use the stellar mass-luminosity relation and present day stellar luminosity function together with a model of how the star formation rate
More informationThe Galaxy Content of Groups and Clusters
The Galaxy Content of Groups and Clusters results from the SDSS Frank van den Bosch (MPIA) in collaboration with Xiaohu Yang (SHAO), Houjun Mo (UMass), Simone Weinmann (Zurich) Surhud More (MPIA), Marcello
More informationGlobular Clusters: hot stellar populations and internal dynamics
Globular Clusters: hot stellar populations and internal dynamics Giornate dell Osservatorio, Bologna 18-19 February 2016 Emanuele Dalessandro Globular clusters: I. hot stellar populations OABO people involved:
More informationMethods of Measuring Black Hole Masses: Reverberation Mapping. Misty C. Bentz Georgia State University
Methods of Measuring Black Hole Masses: Reverberation Mapping Misty C. Bentz Georgia State University Black Hole Masses in AGNs Dynamical methods generally not feasible in AGNs AGNs rare = distant, poor
More informationStellar Populations in the Galaxy
Stellar Populations in the Galaxy Stars are fish in the sea of the galaxy, and like fish they often travel in schools. Star clusters are relatively small groupings, the true schools are stellar populations.
More informationGas Accretion & Outflows from Redshift z~1 Galaxies
Gas Accretion & Outflows from Redshift z~1 Galaxies David C. Koo Kate Rubin, Ben Weiner, Drew Phillips, Jason Prochaska, DEEP2, TKRS, & AEGIS Teams UCO/Lick Observatory, University of California, Santa
More informationThe near-ir stellar populations of active galaxies
Future & Science of Gemini Observatory Toronto 2015 The near-ir stellar populations of active galaxies Rogério Riffel riffel@ufrgs.br FSG15 Toronto, Canada 1 Motivation The NIR stellar content of active
More informationThe overall uncertainty of single-epoch virial black hole mass estimates and its implication to the M BH -σ relation
The overall uncertainty of single-epoch virial black hole mass estimates and its implication to the M BH -σ relation and Daeseong Park Seoul National University E-mail: woo@astro.snu.ac.kr, pds2001@astro.snu.ac.kr
More informationQuantifying the (Late) Assembly History of Galaxies. Michael Pierce (University of Wyoming)
Quantifying the (Late) Assembly History of Galaxies Michael Pierce (University of Wyoming) What I Think We Already Know: Morphology Density Relation (Assembly Depends on Environment) (Dressler 1980) Ratio
More informationGALAXY EVOLUTION STUDIES AND HIGH PERFORMANCE COMPUTING
GALAXY EVOLUTION STUDIES AND HIGH PERFORMANCE COMPUTING Andreas Efstathiou European University Cyprus Astrophysics and HPC group ACTIVE AREAS OF ASTRONOMY OPPORTUNITIES FOR THEORETICAL, OBSERVATIONAL AND
More informationFeeding the Beast. Chris Impey (University of Arizona)
Feeding the Beast Chris Impey (University of Arizona) Note: the box is growing due to cosmic expansion but this is factored out. Heirarchical Structure Active Galactic Nuclei (AGN) Nuclear activity in
More informationClusters of Galaxies with Euclid
Clusters of Galaxies with Euclid Figure by L. Caridà A. Biviano (INAF-OATS) largely based on Sartoris, AB, Fedeli et al. 2016 Euclid: ESA medium class A&A mission, selected Oct 2011, to be launched in
More informationStellar Populations: Resolved vs. unresolved
Outline Stellar Populations: Resolved vs. unresolved Individual stars can be analyzed Applicable for Milky Way star clusters and the most nearby galaxies Integrated spectroscopy / photometry only The most
More informationA Strongly Lensed Massive Quiescent Galaxy at z=2.63: of
A Strongly Lensed Massive Quiescent Galaxy at z=2.63: Indica@ons of Rota@on Drew Newman Carnegie Ins@tu@on for Science November 17, 2015 / Yale Collaborators: Sirio Belli, Richard Ellis Resolving the kinema@cs
More informationSTRUCTURE AND DYNAMICS OF GALAXIES
STRUCTURE AND DYNAMICS OF GALAXIES 14. Piet van der Kruit Kapteyn Astronomical Institute University of Groningen, the Netherlands www.astro.rug.nl/ vdkruit Beijing, September 2011 The fundamental discussion
More informationHigh-redshift galaxies
High-redshift galaxies Houjun Mo May 4, 2004 Galaxies can now be observed to z 6 Normal galaxies with 0.2 < z < 1 The Lyman-break population at z 3 The sub-mm sources at z 3 Between 1 2, spectroscopy desert,
More informationFrom theory to observations
Stellar Objects: From theory to observations 1 From theory to observations Given the stellar mass and chemical composition of a ZAMS, the stellar modeling can, in principle, give the prediction of the
More informationHow environment shapes galaxy evolution: the satellite galaxies' perspective
How environment shapes galaxy evolution: the satellite galaxies' perspective Anna Pasquali Astronomisches Rechen Institut, Zentrum für Astronomie der Universität Heidelberg NGC 4651 Why do we care? At
More informationMonolithic View of Galaxy Formation and Evolution
Galaxies 2014, 2, 300-381; doi:10.3390/galaxies2030300 OPEN ACCESS galaxies ISSN 2075-4434 www.mdpi.com/journal/galaxies Review Monolithic View of Galaxy Formation and Evolution Cesare Chiosi 1, *, Emiliano
More informationGalaxies Across Cosmic Time
Galaxies Across Cosmic Time Overview: 1. Epoch of Reionization (z>6) 2. Stellar Mass Functions to z~6 3. Deep Spectroscopy at z~2-3 4. Circumgalactic Medium (z
More informationBridging the near and the far: constraints on first star formation from stellar archaeology. Raffaella Schneider Sapienza University of Rome
Bridging the near and the far: constraints on first star formation from stellar archaeology Raffaella Schneider Sapienza University of Rome Kyoto,First Stars IV 2012 Kyoto,First Stars IV 2012 "As we extend
More informationDetermination of [α/fe] and its Application to SEGUE F/G Stars. Young Sun Lee
Determination of [α/fe] and its Application to SEGUE F/G Stars Young Sun Lee Research Group Meeting on June 16, 2010 Outline Introduction Why [α/fe]? Determination of [α/fe] Validation of estimate of [α/fe]
More informationReview of stellar evolution and color-magnitude diagrams
Review of stellar evolution and color-magnitude diagrams The evolution of stars can be used to study the properties of galaxies Very characteristic features pinpoint at the age (chemistry) of the stars
More informationThe non-universal Initial Mass Function of early-type galaxies. Francesco La Barbera INAF-Osservatorio Astronomico di Capodimonte
The non-universal Initial Mass Function of early-type galaxies Francesco La Barbera INAF-Osservatorio Astronomico di Capodimonte The stellar Initial Mass Function (IMF) The stellar IMF is the mass distribution
More informationStar Formation. Answering Fundamental Questions During the Spitzer Warm Mission Phase
Star Formation Answering Fundamental Questions During the Spitzer Warm Mission Phase Lori Allen CfA John Carpenter, Caltech Lee Hartmann, University of Michigan Michael Liu, University of Hawaii Tom Megeath,
More informationReverberation Mapping in the Era of MOS and Time-Domain Surveys: from SDSS to MSE
Reverberation Mapping in the Era of MOS and Time-Domain Surveys: from SDSS to MSE Yue Shen Carnegie Obs -> University of Illinois at Urbana-Champaign MSE Science Team Meeting, July 29-31 2015, Big Island
More informationSLACS Spectroscopy. Observations, Kinematics & Stellar Populations. Oliver Czoske Kapteyn Institute, Groningen, NL
SLACS Spectroscopy Observations, Kinematics & Stellar Populations Oliver Czoske Kapteyn Institute, Groningen, NL Strong Gravitational Lensing in the Next Decade Cogne, 22 June 2009 Collaborators Léon Koopmans
More informationLya as a Probe of the (High-z) Universe
Lya as a Probe of the (High-z) Universe Mark Dijkstra (CfA) Main Collaborators: Adam Lidz, Avi Loeb (CfA) Stuart Wyithe (Melbourne), Zoltan Haiman (Columbia) Lya as a Probe of the (High-z) Universe Outline
More informationCOLOR SEPARATION OF GALAXY TYPES IN THE SLOAN DIGITAL SKY SURVEY IMAGING DATA
COLOR SEPARATION OF GALAXY TYPES IN THE SLOAN DIGITAL SKY SURVEY IMAGING DATA Strateva et al. 2001, AJ, 122, 1861 Presenter: Ken Mawatari Date: 2011 October 31 2011/10/31 1 Outline Abstruct : roughly Introduction
More informationCharacterising the last 8 Gyr. The present-day Universe
Characterising the last 8 Gyr The present-day Universe 1 Luminosity and mass functions Redshift survey Apparent magnitude limited e.g., SDSS 14.5
More informationGlobular Clusters in LSB Dwarf Galaxies
Globular Clusters in LSB Dwarf Galaxies New results from HST photometry and VLT spectroscopy Thomas H. Puzia Herzberg Institute of Astrophysics in collaboration with Margarita E. Sharina SAO, Russian Academy
More informationEmpirical Evidence for AGN Feedback
Empirical Evidence for AGN Feedback Christy Tremonti MPIA (Heidelberg) / U. Wisconsin-Madison Aleks Diamond-Stanic (U. Arizona), John Moustakas (NYU) Much observational and theoretical evidence supports
More informationScience with the Intermediate Layer
Science with the Intermediate Layer 20 deg 2 to depth of grizy=28.6,28.1,27.7,27.1,26.6 10 7 Mpc 3 at z 2 Jenny E. Greene (Princeton/Carnegie, Hubble Fellow) Watching Galaxies Assemble Thomas et al. 2005
More informationGalaxy formation and evolution. Astro 850
Galaxy formation and evolution Astro 850 Introduction What are galaxies? Systems containing many galaxies, e.g. 10 11 stars in the Milky Way. But galaxies have different properties. Properties of individual
More informationUpcoming class schedule
Upcoming class schedule Thursday March 15 2pm AGN evolution (Amy Barger) th Monday March 19 Project Presentation (Brad) nd Thursday March 22 postponed to make up after spring break.. Spring break March
More information