Jens Melinder. With financial support from CNES/CNRS convention #
|
|
- Franklin Wiggins
- 5 years ago
- Views:
Transcription
1 Jens Melinder With financial support from CNES/CNRS convention #
2 u u u u
3 The Lyman-α line in emission u The hydrogen Lyman-α emission line is the intrinsically brightest spectral feature from star-forming galaxies u Early attempts to detect the line in emission were largely unsuccessful. u The resonant nature of Lyα makes radiative transfer effects extremely important. u The escape fraction is often lower than what would be expected from observed nebular extinction. Lyα luminosities do not correlate well with global SFR Meier & Terlevich, 1981
4 Earlier imaging studies of Lyman-α in nearby galaxies Six starburst galaxies observed with HST/ACS (Östlin et al. 2009) u Showed that Lyα scattered out into a halo for the galaxies with net emission.two absorbers, four emitters. u Lack of extinction maps made it hard to account for nebular continuum in the continuum subtraction, and difficult to study the effect of dust on Lyα emission.
5 The original LARS The first 14 galaxies observed within the project showed that Lyα was found in emission in almost all cases (12/14) for a high SFR sample. Again, the imaging showed that Lyα scattered far out from where the photons were produced. u Imaging presented in Hayes et al. (2013, 2014), Östlin et al. (2014), Guaita et al u COS spectroscopy, Duval et al. (2016), Rivera Thorsen et al. (2015), u VLA HI observations, Pardy et al. (2015) u IFU spectroscopy, Herenz et al. (2016)
6 Jens Melinder Veronica Menacho (Stockholm) Matteo Messa (Stockholm) Johannes Puschnig (Stockholm)
7 The primary goals are to return detailed observations of the H I Lyα emission line, and to do so in a sample that is simultaneously as free from bias as possible, statistically meaningful enough to observe trends within the sample, and comparable in selection to galaxies observed in the high-z universe. Hayes et al. (2013) u 14 galaxies in the original LARS with EW(Hα)>100 Å + 28 galaxies with lower ssfr in elars at 0.027<z<0.14. Resolution ~ pc. u 5 blue compact dwarfs observed earlier (e.g. Haro 11, ESO 338-IG04) at 0.09<z< Tol u 5 ULIRGs at z~0.15
8 With ELARS the sample selection was relaxed to include galaxies with EW(Hα)>40 Å, and galaxies fainter in the UV. This selection targets galaxies that are expected to have lower EW(Lα). LARS
9 u Observing nearby galaxies in Lyαallow us to study the faintest emitters. u But are the nearby emitters similar to high redshift LAEs? u The original LARS galaxies are Lyman Break analogues, but ELARS contain more normal spiral galaxies. log Ly Luminosity [ erg s 1 ] C11 W14 G11 H10 C12 B11 R08 H15 LARS elars Redshift References: C11: Cowie et al. 2011, G11: Guaita et al. 2011, C12: Cantalupo et al. 2012, R08: Rauch et al. 2008, W14: Wold et al. 2014, H10: Hayes et al. 2010, B11: Blanc et al. 2011, H15: Henry et al. 2015
10 Observations HST Imaging u 3 FUV broadband filters (ACS/SBC) u 3 optical broadband filters (ACS/WFC3) u 2 NB filters for Hβand Hα(ACS/ WFC3) Other observations u Spectroscopy with COS (see talk by M. Hayes). u VLA/GBT H I of LARS+eLARS (see talk by M. Hayes) u Ground-based optical/nir imaging (NOT/CFHT) u IFU spectroscopy with PMAS and MUSE (see talk by C. Herenz)
11 LARS data reduction and line subtraction Reduced data AstroDrizzle, Cosmic rays Registration Generate PSF models PSF matching SDSS: NII, Z LaXs Lyα, Hα and Hβ line maps. SED fitted age and E(B-V) s maps
12 Continuum subtraction using LaXs Pixel SED fitting using 2 FUV filters and 3 optical broadband filters. Standard Χ 2 fitting on each pixel. u Starburst99 template spectra. u 3-4 free parameters, age of stellar population, stellar extinction, and stellar mass. u Two stellar populations, young+old. u Use extinction corrected Hαto estimate the nebular continuum. u Assumptions: Calzetti attenuation, Z and NII from SDSS, SSP SF history.
13 Lyα FUV Cont. Hα
14 Lyα FUV Cont. Hα
15 Lyα FUV Cont. Hα
16 LARS05 Typical Lyman α emitting galaxy in the original LARS. Quite compact dwarf irregular galaxy with some dust. Lyα seems to escape transverse to the major axis. EW(Hα) 314 Å EW(Lα) 30 Å f esc (Lα) 0.22 M L(FUV) 8e9 M 3.6e40 erg/s/å E(B-V) n 0.11
17 LARS05 Typical Lyman α emitting galaxy in the original LARS. Quite compact dwarf irregular galaxy with some dust. Lyα seems to escape transverse to the major axis. EW(Hα) 314 Å EW(Lα) 30 Å f esc (Lα) 0.22 M L(FUV) 8e9 M 3.6e40 erg/s/å E(B-V) n 0.11
18 ELARS01/NGC 6090 Galaxy merger and LIRG.Contains significant amounts of dust, but Lyα manages to escape even in the center of the system, maybe because of a patchy ISM structure. EW(Hα) 120 Å EW(Lα) 15 Å f esc (Lα) M L(FUV) E(B-V) n e10 M 4.0e40 erg/s/å
19 ELARS01/NGC 6090 Galaxy merger and LIRG.Contains significant amounts of dust, but Lyα manages to escape even in the center of the system, maybe because of a patchy ISM structure. EW(Hα) 120 Å EW(Lα) 15 Å f esc (Lα) M L(FUV) E(B-V) n e10 M 4.0e40 erg/s/å
20 ELARS10 Spiral galaxy at quite low inclination with significant dust. This system is a net absorber, but some Lyα radiation is able to escape from starforming regions in the arms. EW(Hα) 48 Å EW(Lα) -11 Å f esc (Lα) 0.0 M L(FUV) 3e10 M 1.4e40 erg/s/å E(B-V) n 0.27
21 ELARS10 Spiral galaxy at quite low inclination with significant dust. This system is a net absorber, but some Lyα radiation is able to escape from starforming regions in the arms. EW(Hα) 48 Å EW(Lα) -11 Å f esc (Lα) 0.0 M L(FUV) 3e10 M 1.4e40 erg/s/å E(B-V) n 0.27
22 Global measurements on LARS galaxies u Comparing two different apertures, both based on isophotal analysis of the line and continuum maps. - One aperture with an equivalent radius of 2 times the petrosian radius (estimated from the continuum UV map) - The other based on the faintest detectable isophotes in Lyα and continuum UV. u Errors from Monte Carlo simulations of the continuum subtraction. This is work in progress.
23 Lyα spatial distribution <2 r p20 > = 5 kpc <r totmask > =13 kpc Escape fractions may be severely underestimated when using smaller apertures. The fraction of net Lyα emitters in LARS/ELARS is: 35(12)/42 for a mask designed to include all Lyα (with EW(Lyα)>20) 29(11)/42 for a 2 r p20 radius aperture (with EW(Lyα)>20)
24 Lyα spatial distribution Do more extended Lyα emitters have higher escape fraction? -> No proper correlation found.
25 Lyα equivalent width distributions u The Lyα emitters with high escape fractions have the highest equivalent widths. u Galaxies with high EW(Lyα) all have low E(B-V) neb
26 Lyα equivalent width distributions u Low EW(Hα) (low ssfr) galaxies all have lower EW(Lyα) u High mass galaxies have low EW(Lyα)
27 How dust affects the escape fraction. Dust geometry Radiative transfer
28 Summary u Figuring out how and how and when Lyα radiation can escape is important for high redshift studies and can also give useful information about the ISM in star forming galaxies. u LARS is a sample of ~50 star-forming galaxies at z<0.15 with multi-wavelength observations available. The back-bone is the FUV-optical HST observations. u Lyα escape is mediated not by a single parameter, but by many different factors. Dust and neutral gas and how these components are distributed, as well as gas kinematics are important. All calibrated/stacked HST data and line maps for the 42 LARS galaxies will be released to the community in 2017.
Emission Lyα dans les galaxies starburst
Emission Lyα dans les galaxies starburst D. Kunth, D. Schaerer; M. Hayes; G. Ostlin, J.M. Mas-Hesse; A. Verhamme; C. Leitherer; A. Petrosian Institut d'astrophysique de Paris Atelier MUSE Lyon, 7- Lyα
More informationAlaina Henry Goddard Space Flight Center
Lyman α emission from Green Peas The Role of Circumgalactic Gas Density, Covering, and Kinematics Alaina Henry Goddard Space Flight Center Imaged Lyα from a Green Pea galaxy Hayes et al. (2014) Claudia
More informationA study of extended Lyman alpha halos around galaxies
A study of extended Lyman alpha halos around galaxies Sourabh Chauhan 1 1 MIFA, UMN, Minnesota (Dated: July 5, 2016) PACS numbers: INTRODUCTION Lyman alpha emitters have been extensively studied[2] and
More informationPhysical conditions of the interstellar medium in star-forming galaxies at z~1.5
Physical conditions of the interstellar medium in star-forming galaxies at z~1.5 Abstract Masao Hayashi (NAOJ, Mitaka) Subaru seminar @ Subaru Telescope, NAOJ 10 March 2015 To be re-submitted soon to PASJ
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 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 informationarxiv: v1 [astro-ph.ga] 2 Dec 2015
Astronomy & Astrophysics manuscript no. article c ESO 2015 December 4, 2015 The Lyman alpha Reference Sample VI: Lyman alpha escape from the edge-on disk galaxy Mrk1486 Florent Duval 1,2, Göran Östlin2,
More informationarxiv: v4 [astro-ph] 30 Jul 2009
The Lyman alpha morphology of local starburst galaxies: release of calibrated images Göran Östlin1 Department of Astronomy, Stockholm University, AlbaNova University Center, 10691 Stockholm, Sweden ostlin@astro.su.se
More informationUnderstanding Lyα Emission Using LBGs (and vice versa)
Understanding Lyα Emission Using LBGs (and vice versa) Alice Shapley (UCLA) Collaborators: Kathy Kornei, Kristin Kulas, Juna Kollmeier, Dawn Erb, Anna Quider, Max Pettini, Chuck Steidel z>1.5 Galaxy Identification
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 informationHow extinction correction influences the estimate of Lyα escape fraction?
How extinction correction influences the estimate of Lyα escape fraction? Speaker: Fangxia An (Purple Mountain Observatory; Durham University) fangxiaan@pmo.ac.cn Supervisor: Xianzhong Zheng; Ian Smail;
More informationHigh Redshift Universe
High Redshift Universe Finding high z galaxies Lyman break galaxies (LBGs) Photometric redshifts Deep fields Starburst galaxies Extremely red objects (EROs) Sub-mm galaxies Lyman α systems Finding high
More informationResolved Spectroscopy of Adolescent and Infant Galaxies (1 < z < 10) July 18, 2014 TMT Science Forum, Tucson
Resolved Spectroscopy of Adolescent and Infant Galaxies (1 < z < 10) July 18, 2014 TMT Science Forum, Tucson Shelley Wright (Dunlap Institute, Univ. of Toronto), and IRIS Science Team 1 How does the zoology
More informationPaul Sell. University of Wisconsin-Madison Advisor: Christy Tremonti
A SAMPLE OF EXTREME MERGER-DRIVEN STARBURST GALAXIES AS VIEWED BY THE CHANDRA AND HUBBLE SPACE TELESCOPES Paul Sell University of Wisconsin-Madison Advisor: Christy Tremonti Collaboration: Aleks Diamond-Stanic,
More informationSome HI is in reasonably well defined clouds. Motions inside the cloud, and motion of the cloud will broaden and shift the observed lines!
Some HI is in reasonably well defined clouds. Motions inside the cloud, and motion of the cloud will broaden and shift the observed lines Idealized 21cm spectra Example observed 21cm spectra HI densities
More informationProperties of Lyman-α and Gamma-Ray Burst selected Starbursts at high Redshifts
Properties of Lyman-α and Gamma-Ray Burst selected Starbursts at high Redshifts Johan P. U. Fynbo (University of Copenhagen, jfynbo@astro.ku.dk) Motivation Lyman-α selected startbursts at z=3 Gamma-Ray
More information9. Evolution with redshift - z > 1.5. Selection in the rest-frame UV
11-5-10see http://www.strw.leidenuniv.nl/ franx/college/galaxies10 10-c09-1 11-5-10see http://www.strw.leidenuniv.nl/ franx/college/galaxies10 10-c09-2 9. Evolution with redshift - z > 1.5 Selection in
More informationFaint Lyman Alpha Emission at z~3
Faint Lyman Alpha Emission at z~3 M. Rauch (OCIW) Collaborators ESO data : Haehnelt (IoA), Bunker (Oxford), Becker (KICC), Marleau (IPAC), Graham (UCB), Cristiani (Trieste), Jarvis (Hertfordshire), Lacey
More informationarxiv: v1 [astro-ph.ga] 4 Jun 2018
Astronomy& Astrophysics manuscript no. 32478 c ESO 218 June, 218 Puzzling Lyman-alpha line profiles in green pea galaxies I. Orlitová 1, A. Verhamme 2, A. Henry 3, C. Scarlata 4, A. Jaskot, 6,, M. S. Oey
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 informationGas 1: Molecular clouds
Gas 1: Molecular clouds > 4000 known with masses ~ 10 3 to 10 5 M T ~ 10 to 25 K (cold!); number density n > 10 9 gas particles m 3 Emission bands in IR, mm, radio regions from molecules comprising H,
More informationSeeing Through the Trough: Detecting Lyman Alpha from Early Generations of Galaxies
Seeing Through the Trough: Detecting Lyman Alpha from Early Generations of Galaxies Mark Dijkstra (ITC) collaborators: Stuart Wyithe, Avi Loeb, Adam Lidz, Zoltan Haiman Schematic History of the Universe
More informationBlack Holes and Active Galactic Nuclei
Black Holes and Active Galactic Nuclei A black hole is a region of spacetime from which gravity prevents anything, including light, from escaping. The theory of general relativity predicts that a sufficiently
More informationDust properties of galaxies at redshift z 5-6
Dust properties of galaxies at redshift z 5-6 Ivana Barisic 1, Supervisor: Dr. Peter L. Capak 2, and Co-supervisor: Dr. Andreas Faisst 2 1 Physics Department, University of Zagreb, Zagreb, Croatia 2 Infrared
More informationLyα AND UV SIZES OF GREEN PEA GALAXIES
Draft version July 8, 17 Preprint typeset using L A TEX style emulateapj v. 1/3/15 Lyα AND UV SIZES OF GREEN PEA GALAXIES Huan Yang 1,, Sangeeta Malhotra, James E. Rhoads, Claus Leitherer 3, Aida Wofford
More informationDust in dwarf galaxies: The case of NGC 4214
Dust in dwarf galaxies: The case of NGC 4214 Ute Lisenfeld Israel Hermelo Monica Relaño Richard Tuffs Cristina Popescu Joerg Fischera Brent Grove Image from HST WFC3 (Image: NASA/ESA/Hubble Heritage) Dust
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 informationarxiv: v1 [astro-ph.ga] 7 Oct 2015
Title of your IAU Symposium Proceedings IAU Symposium No. 316, 2015 A.C. Editor, B.D. Editor & C.E. Editor, eds. c 2015 International Astronomical Union DOI: 00.0000/X000000000000000X The super star cluster
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 informationDLAs Probing Quasar Host Galaxies. Hayley Finley P. Petitjean, P. Noterdaeme, I. Pâris + SDSS III BOSS Collaboration 2013 A&A
DLAs Probing Quasar Host Galaxies Hayley Finley P. Petitjean, P. Noterdaeme, I. Pâris + SDSS III BOSS Collaboration 2013 A&A 558 111 Outline Feedback mechanisms in QSO host galaxies Strong DLAs at zqso
More informationA Local Clue to the Reionization of the Universe
A Local Clue to the Reionization of the Universe arxiv:1410.3511v1 [astro-ph.ga] 13 Oct 2014 Sanchayeeta Borthakur, 1 Timothy M. Heckman, 1 Claus Leitherer, 2 Roderik A. Overzier 3 1 Center for Astrophysical
More informationIonized and atomic interstellar medium in star-forming galaxies. Thøger Emil Rivera-Thorsen
Ionized and atomic interstellar medium in star-forming galaxies Thøger Emil Rivera-Thorsen Ionized and atomic interstellar medium in star-forming galaxies Thøger Emil Rivera-Thorsen Cover image: 2D spectrum
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 informationActive Galaxies & Emission Line Diagnostics
Active Galaxies & Emission Line Diagnostics Review of Properties Discussed: 1) Powered by accretion unto a supermassive nuclear black hole 2) They are the possible precursors to luminous massive galaxies
More information- AGN feedback in action?
Gas outflows and star formation in type 2 AGNs - AGN feedback in action? Jong-Hak Woo (Seoul National Univ.) & Hyun-Jin Bae, Donghoon Son, Marios Karouzos Muse view of OIII outflows in NGC 7582 (Juneau+16
More informationA mid and far-ir view of the star formation activity in galaxy systems and their surroundings
A mid and far-ir view of the star formation activity in galaxy systems and their surroundings Andrea Biviano Andrea Biviano INAF/Osservatorio Astronomico di Trieste Outline: mid-ir & multiwavelength observations
More informationarxiv: v1 [astro-ph] 22 May 2008
Astronomy & Astrophysics manuscript no. Atek Lya astroph c ESO 2008 May 22, 2008 arxiv:0805.3501v1 [astro-ph] 22 May 2008 On the detectability of Lyα emission in star-forming galaxies The role of dust
More informationNeon Emission in HST Emission- Line Galaxies at z 2. Greg Zeimann
Neon Emission in HST Emission- Line Galaxies at z 2 Greg Zeimann grzeimann@psu.edu Using radia@ve transfer modeling to infer the physical condi@ons of the warm ionized gas and the ionizing source Modeling
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 informationarxiv: v1 [astro-ph.ga] 13 Sep 2016
Draft version May 10, 018 Preprint typeset using L A TEX style emulateapj v. 5//11 DETECTION OF HI IN EMISSION IN THE LYMAN ALPHA EMITTING GALAXY HARO 11 Stephen A. Pardy Department of Astronomy, University
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 informationEmission lines in star-forming galaxies
Emission lines in star-forming galaxies Daniel Schaerer (Geneva Observatory & CNRS) Introduction Properties of CIII] and CIV emitters at high redshift Compact strong emission line galaxies at z~0.3: analogs
More informationM.Phys., M.Math.Phys., M.Sc. MTP Radiative Processes in Astrophysics and High-Energy Astrophysics
M.Phys., M.Math.Phys., M.Sc. MTP Radiative Processes in Astrophysics and High-Energy Astrophysics Professor Garret Cotter garret.cotter@physics.ox.ac.uk Office 756 in the DWB & Exeter College Radiative
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 informationarxiv: v2 [astro-ph.ga] 5 Mar 2015
Accepted for publication in ApJ Preprint typeset using L A TEX style emulateapj v. 5/2/11 THE LYMAN ALPHA REFERENCE SAMPLE: V. THE IMPACT OF NEUTRAL ISM KINEMATICS AND GEOMETRY ON LYMAN ALPHA ESCAPE Thøger
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 informationMeasuring stellar distances.
Measuring stellar distances This method can be used to measure distances up to 100pc Some new technology allows measuring distances up to 200pc using this method p= 1/d Stellar Parallax.htm This method
More informationLecture 15: Galaxy morphology and environment
GALAXIES 626 Lecture 15: Galaxy morphology and environment Why classify galaxies? The Hubble system gives us our basic description of galaxies. The sequence of galaxy types may reflect an underlying physical
More informationRevealing new optically-emitting extragalactic Supernova Remnants
10 th Hellenic Astronomical Conference Ioannina, September 2011 Revealing new optically-emitting extragalactic Supernova Remnants Ioanna Leonidaki (NOA) Collaborators: P. Boumis (NOA), A. Zezas (UOC, CfA)
More informationWhat lensed galaxies can tell us about winds, hot stars, and physical conditions
What lensed galaxies can tell us about winds, hot stars, and physical conditions! z=2.161 z=3.066 Jane Rigby!! JWST Deputy Project Scientist for Operations! NASA Goddard Space Flight Center! I ll talk
More informationThe First Galaxies. Erik Zackrisson. Department of Astronomy Stockholm University
The First Galaxies Erik Zackrisson Department of Astronomy Stockholm University Outline The first galaxies what, when, why? What s so special about them? Why are they important for cosmology? How can we
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 informationA Far-ultraviolet Fluorescent Molecular Hydrogen Emission Map of the Milky Way Galaxy
A Far-ultraviolet Fluorescent Molecular Hydrogen Emission Map of the Milky Way Galaxy (The Astrophysical Journal Supplement Series, 231:21 (16pp), 2017 August) November 14, 2017 Young-Soo Jo Young-Soo
More informationA TALE OF TWO MONSTERS: EMBEDDED AGN IN NGC6418 AND IRAS
A TALE OF TWO MONSTERS: EMBEDDED AGN IN NGC6418 AND IRAS16399 0937 Photometry Aperture 2.2 2.0 1.8 Optical 3.6 µm E 4.5 µm N Normalized flux 1.6 1.4 0 100 200 300 Figure 3.1: NGC6418 false color image
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 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 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 informationGas in and around z > 2 galaxies
Gas in and around z > 2 galaxies Michele Fumagalli August 2010 Santa Cruz Xavier Prochaska Daniel Kasen Avishai Dekel In collaboration with: Daniel Ceverino Joel Primack Gas in galaxies from theory Gas
More informationLyman alpha Emitters and Typical Galaxies at High Redshift
Lyman alpha Emitters and Typical Galaxies at High Redshift M. Rauch (OCIW) Collaborators: Haehnelt (IoA), Bunker (Oxford), Becker (OCIW), Marleau (IPAC), Graham (UCB), Cristiani (Trieste), Jarvis (Hertfordshire),
More informationThe relation between cold dust and star formation in nearby galaxies
The relation between cold dust and star formation in nearby galaxies George J. Bendo (with the Herschel Local Galaxies Guaranteed-Time Surveys and the Herschel Virgo Cluster Survey) Outline Analyses before
More informationProbing the End of Dark Ages with High-redshift Quasars. Xiaohui Fan University of Arizona Dec 14, 2004
Probing the End of Dark Ages with High-redshift Quasars Xiaohui Fan University of Arizona Dec 14, 2004 High-redshift Quasars and the End of Cosmic Dark Ages Existence of SBHs at the end of Dark Ages BH
More informationX-ray emission from star-forming galaxies
X-ray emission from star-forming galaxies, Marat Gilfanov & Rashid Sunyaev (Max Planck Institute for Astrophysics) Ultra-Luminous X-ray sources and Middle Weight Black Holes Monday May 24th, 2010 - ESAC
More informationAnatomy of an X-ray detected cluster at z = 2: low metallicities and enhanced specific star formation rates in star-forming galaxies.
Anatomy of an X-ray detected cluster at z = 2: low metallicities and enhanced specific star formation rates in star-forming galaxies. F. Valentino 1, E. Daddi 1, V. Strazzullo 1,2, R. Gobat 1,3, F. Bournaud
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 information68 Star Formation Laws in LITTLE THINGS Dwarfs: The case of DDO133 and DDO168. Dana Ficut-Vicas
68 Star Formation Laws in LITTLE THINGS Dwarfs: The case of DDO133 and DDO168 Dana Ficut-Vicas Little Things Project LITTLE: Local Irregulars That Trace Luminosity Extremes THINGS: The HI Nearby Galaxy
More informationHigh-Redshift Galaxies: A brief summary
High-Redshift Galaxies: A brief summary Brant Robertson (Caltech) on behalf of David Law (UCLA), Bahram Mobasher (UCR), and Brian Siana (Caltech/Incoming CGE) Observable Cosmological History t~3.7x10 5
More informationAndromeda in all colours
Andromeda in all colours Sébastien Viaene and the HELGA team: J. Fritz, M. Baes, G.J. Bendo, J.A.D.L. Blommaert, M. Boquien, A. Boselli, L. Ciesla, L. Cortese, I. De Looze, W.K. Gear, G. Gentile, T.M.
More informationComponents of Galaxies Gas The Importance of Gas
Components of Galaxies Gas The Importance of Gas Fuel for star formation (H 2 ) Tracer of galaxy kinematics/mass (HI) Tracer of dynamical history of interaction between galaxies (HI) The Two-Level Atom
More informationEnergy Sources of the Far IR Emission of M33
Energy Sources of the Far IR Emission of M33 Hinz, Reike et al., ApJ 154: S259 265 (2004). Presented by James Ledoux 24 µm 70 µm 160 µm Slide 1 M33 Properties Distance 840kpc = 2.7 Mlyr (1'' ~ 4 pc) Also
More informationSTAR FORMATION RATES observational overview. Ulrike Kuchner
STAR FORMATION RATES observational overview Ulrike Kuchner Remember, remember.. Outline! measurements of SFRs: - techniques to see what the SF rate is - importance of massive stars and HII regions - the
More informationAGN Physics of the Ionized Gas Physical conditions in the NLR Physical conditions in the BLR LINERs Emission-Line Diagnostics High-Energy Effects
AGN Physics of the Ionized Gas Physical conditions in the NLR Physical conditions in the BLR LINERs Emission-Line Diagnostics High-Energy Effects 1 Evidence for Photoionization - continuum and Hβ luminosity
More informationGalaxies 626. Lecture 10 The history of star formation from far infrared and radio observations
Galaxies 626 Lecture 10 The history of star formation from far infrared and radio observations Cosmic Star Formation History Various probes of the global SF rate: ρ* (z) M yr 1 comoving Mpc 3 UV continuum
More informationarxiv: v1 [astro-ph.ga] 10 Sep 2018
Astronomy & Astrophysics manuscript no. E338feedback c ESO 2018 September 12, 2018 Super star cluster feedback driving ionization, shocks and outflows in the halo of the nearby starburst ESO 338-IG04 A.
More informationDusty star-forming galaxies at high redshift (part 5)
Dusty star-forming galaxies at high redshift (part 5) Flow of story 4.1.1 4.1.2 4.1.3 Millimetric Spectroscopic Redshifts Millimetric Photometric Redshifts Redshift Distributions of 24 μm selected DSFG
More informationUnveiling the nature of bright z ~ 7 galaxies with HST and JWST
Unveiling the nature of bright z ~ 7 galaxies with HST and JWST Rebecca Bowler Hintze Fellow, University of Oxford Nicholas Kurti Junior Fellow, Brasenose College with Jim Dunlop, Ross McLure, Derek McLeod,
More informationMultiwavelength Study of Distant Galaxies. Toru Yamada (Subaru Telescope, NAOJ)
Multiwavelength Study of Distant Galaxies Toru Yamada (Subaru Telescope, NAOJ) Studying Galaxy Formation with ALMA 1. Studying Galaxy Forming Region with ALMA 2. Multi-wavelength Study of Galaxy Formation/Evolution
More informationThe Milky Way. Overview: Number of Stars Mass Shape Size Age Sun s location. First ideas about MW structure. Wide-angle photo of the Milky Way
Figure 70.01 The Milky Way Wide-angle photo of the Milky Way Overview: Number of Stars Mass Shape Size Age Sun s location First ideas about MW structure Figure 70.03 Shapely (~1900): The system of globular
More informationLecture 11: SDSS Sources at Other Wavelengths: From X rays to radio. Astr 598: Astronomy with SDSS
Astr 598: Astronomy with SDSS Spring Quarter 4, University of Washington, Željko Ivezić Lecture : SDSS Sources at Other Wavelengths: From X rays to radio Large Surveys at Many Wavelengths SDSS: UV-IR five-band
More informationTest #1! Test #2! Test #2: Results!
High-Redshift Galaxies II - Populations (cont d) - Current Redshift Frontier - Gravitational Lensing I will hand back Test #2 HW#10 will be due next Monday. Nov 18, 2015 Test #1 Test #2 Test #2: Results
More informationarxiv: v3 [astro-ph.co] 1 Dec 2011
X-ray Constraints on the Lyα Escape Fraction Zhen-Ya Zheng 1,2 ; Sangeeta Malhotra 2 ; Jun-Xian Wang 1 ; James E. Rhoads 2 ; Steven L. Finkelstein 3 ; Eric Gawiser 4 ; Caryl Gronwall 5 ; Lucia Guaita 6
More informationLecture Two: Galaxy Morphology:
Lecture Two: Galaxy Morphology: Looking more deeply at the Hubble Sequence Galaxy Morphology How do you quantify the properties of galaxies? and how do you put them in groups which allow you to study physically
More informationInvestigating the connection between LyC and Lyα emission and other indirect indicators
Investigating the connection between LyC and Lyα emission and other indirect indicators F. Marchi, L. Pentericci, L. Guaita, D. Schaerer, M. Castellano, B. Ribeiro and the VUDS collaboration Emission line
More informationInterpreting Galaxies across Cosmic Time with Binary Population Synthesis Models
Interpreting Galaxies across Cosmic Time with Binary Population Synthesis Models Elizabeth Stanway Warwick (UK) with J J Eldridge (Auckland, NZ) and others Putting Warwick on the Map WARWICK! London @WarwickAstro
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 informationLecture 27 The Intergalactic Medium
Lecture 27 The Intergalactic Medium 1. Cosmological Scenario 2. The Ly Forest 3. Ionization of the Forest 4. The Gunn-Peterson Effect 5. Comment on HeII Reionization References J Miralda-Escude, Science
More informationarxiv: v1 [astro-ph.co] 7 Sep 2011
Mon. Not. R. Astron. Soc. 000, 1?? (2002) Printed 8 September 2011 (MN LATEX style file v2.2) arxiv:1109.1333v1 [astro-ph.co] 7 Sep 2011 The properties of the brightest Lyα emitters at z 5.7 C. Lidman,
More informationJWST Extragalactic Mock Catalog Documentation
JWST Extragalactic Mock Catalog Documentation Version 1.1 Kevin Hainline Emma Curtis-Lake Christina Williams Jacopo Chevallard Last Update: May 23, 2018 Contents 1 Introduction 2 1.1 Mock catalog overview.....................................
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 informationThe Puzzle of the Lya Galaxies: New Results from the VLT
Astronomical Science The Puzzle of the Lya Galaxies: New Results from the VLT Christian Tapken 1 Immo Appenzeller 2 Armin Gabasch 3, 4, Jochen Heidt 2 Ulrich Hopp 3, 4 Ralf Bender 3, 4 Stefan Noll 3, 4
More informationAtomic Physics and the Kramers-Heisenberg Formula for Ly Alpha. Hee-Won Lee Department of Physics and Astrnomy Sejong University January 24, 2019
Atomic Physics and the Kramers-Heisenberg Formula for Ly Alpha Hee-Won Lee Department of Physics and Astrnomy Sejong University January 24, 2019 Contents 1. Introduction Quasar Absorption Systems and Cosmic
More informationX-raying galactic feedback in nearby disk galaxies. Q. Daniel Wang University of Massachusetts
X-raying galactic feedback in nearby disk galaxies Q. Daniel Wang University of Massachusetts Chandra survey of diffuse X-ray emission from 53 edge-on galaxies i > 60 o, D < 30 Mpc (Li, J.-T. & Wang, Q.D.
More informationLuminosity Functions of Planetary Nebulae & Globular Clusters. By Azmain Nisak ASTR 8400
Luminosity Functions of Planetary Nebulae & Globular Clusters By Azmain Nisak ASTR 8400 Calculating Distance! m = apparent magnitude! M = absolute magnitude! r = distance in pc GLOBULAR CLUSTERS AS DISTANCE
More informationStellar populations of quasar host galaxies
Knud Jahnke AIP Galaxies division Hauskolloquium 10.01.2003 Introduction/motivation Multicolour imaging On-nucleus spectroscopy What does this teach us? Outlook Overview Introduction Introduction HE 1043
More informationExploiting Cosmic Telescopes with RAVEN
Exploiting Cosmic Telescopes with RAVEN S. Mark Ammons Lawrence Livermore National Laboratory Thanks to: Ken Wong (Arizona) Ann Zabludoff (Arizona) Chuck Keeton (Rutgers) K. Decker French (Arizona) RAVEN
More informationThe First Billion Year of History - Galaxies in the Early Universe. Stephen Wilkins, Silvio Lorenzoni, Joseph Caruana, Holly Elbert, Matt Jarvis
The First Billion Year of History - Galaxies in the Early Universe Stephen Wilkins, Silvio Lorenzoni, Joseph Caruana, Holly Elbert, Matt Jarvis X recent z=8.3 GRB CCDs HST Keck Subaru Picture credit:
More informationTHE FIRST DEEP ADVANCED CAMERA FOR SURVEYS Ly IMAGES OF LOCAL STARBURST GALAXIES Daniel Kunth. Claus Leitherer. J. Miguel Mas-Hesse 1
The Astrophysical Journal, 597:263 268, 2003 November 1 # 2003. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE FIRST DEEP ADVANCED CAMERA FOR SURVEYS Ly IMAGES OF LOCAL STARBURST
More information6. Interstellar Medium. Emission nebulae are diffuse patches of emission surrounding hot O and
6-1 6. Interstellar Medium 6.1 Nebulae Emission nebulae are diffuse patches of emission surrounding hot O and early B-type stars. Gas is ionized and heated by radiation from the parent stars. In size,
More informationStars, Galaxies & the Universe Lecture Outline
Stars, Galaxies & the Universe Lecture Outline A galaxy is a collection of 100 billion stars! Our Milky Way Galaxy (1)Components - HII regions, Dust Nebulae, Atomic Gas (2) Shape & Size (3) Rotation of
More informationGalactic-Scale Winds. J. Xavier Prochaska Inster(stellar+galactic) Medium Program of Studies [IMPS] UCO, UC Santa Cruz.
Galactic-Scale Winds http://arxiv.org/abs/1008.3xxx JXP, Kasen, Rubin, ApJ, to be submitted J. Xavier Prochaska Inster(stellar+galactic) Medium Program of Studies [IMPS] UCO, UC Santa Cruz Kate Rubin (IMPS,
More information