Galaxy Evolution From The Galaxies'
Galaxy evolution from the galaxies’perspective: from gas to stars and back againReinhard Genzel, MPE & UCBLecture 1 gas & star formation in local disk galaxies discourse on observational capabilities, from UV to radioLecture 2 starbursts, mergers & ULIRGs star forming galaxies at the peak of the galaxy formation epoch galaxy kinematics: disks and mergersLecture 3 galaxy kinematics: disks and mergers gas at the peak of the galaxy formation epoch observations of stellar and AGN feedback disk evolution metallicity and metallicity gradients
observational strategies for studyinggalaxy formation/evolution multi-band look-back imaging surveys large samples, but ‘cheap’ proxies local stellar archaeology detailed, spatially resolved in situ observations smallrepresentative samples because ‘expensive’ pathologyHanny’s Vorwerp
gas & star formation in local diskgalaxiesMark Krumholz lectures 1,2see McKee & Ostriker 2007 ARAAKennicutt & Evans 2012 ARAA
star formation in the MW occurs in dusty GiantMolecular Clouds (GMCs)Milky WayBzK/BXULIRG/SMGMcloud103 .106.5107.5 109.5no clouds? Σ(gas) M pc-2200103(N(H) 1022,AV 5)103.5 4.5(N(H) 1024)P/k 19 Σ2(cm-3 K)105.9( MW 105)107.3109.3 (H2) (cm-3)102 .4( MW 1) (km/s)5 cS(10-30 K)25-8050-100M25100-200 200Q0.5-3 10.3 fH2 (MW) [(P/k)/104.4]0.25Taurus GMC CO: Heyer, Goldsmith?103 4 1Herschel PACS/SPIREGMCs are highlystructured ( lognormal densitystructure) withhighly supersoniclocal motions1 l1/2 (Larson 1981)5 2 Rvirialized on large scales 1 but (l R) 1 because Larson relationGMKrumholz et al. 2005,McKee & Ostriker 2007
star formation is inefficientSFR ffM mol gas ff3 n( H ) , where ff 4.3 x106 2 2 32G H 2 10 cm 1/2yrM mol gas ( MW ) 109 M , SFR( MW ) 3M yr 1 ff ( MW ) 0.02 why is star formation so inefficient ?on the other hand gas-depletion M gas 1 2 x109t Hubble ,SFRare galaxies going to stop forming stars tomorrow?two competing explanations:a) MHD pressure (Alfven) prevents collapse on free-fall time scale, which happenson an ambipolar diffusion time scale τambipolar 10-30 τff (Mouschovias, Shu): stars form slowlyb) GMCs are magnetically super-critical but highly super-sonic; because of the log-normaldensity distribution resulting from the interplay between compressing and dispersing shocksonly a small fraction of the gas can collapse at any given time (E.Ostriker, MacLow,Elmegreen, Klessen, Krumholz, McKee): stars form inefficientlytheoretical work and observations over the last decade tend to favor the second explanation.However, this then requires a semi-continuous replenishment of the pervasive turbulent energythroughout clouds (including clouds without much internal SF)Zuckerman & Evans 1974, Williams & McKee 1997, Heyer & Brunt 2004, Elmegreen & Scalo 2004, McKee & Ostriker 2007
star clusters in galaxies70-90% of star formation in the MW occurs in clusters (Lada & Lada 1993)NGC3603: massivestar formingregion in the MilkyWay & local Universe:104 M clusters with 100 O starsThe Antennae galaxies:merging galaxy pair inlocal Universe: 106 M ‘super’ stars clusters with104 O-stars
Surveys of SF in nearby galaxies: SINGS (Kennicutt )/GALEX (Gil de Paz )/THINGS (Walter )/HERACLES(Leroy )
Simon Lilly lecture 1star formation tracersKennicutt 1998, ARAAtracesDisadvantageTechnical issuesHα (or Pα, Brγ)Lyman continuumluminosity and formationrate of recently formedmassive starsregions with AV 1 notsampled, escape of LLyc,ISM physics, traces onlyupper IMFExtinction correction(from Hα/Hβ 2.9in Te 104 K case B)UV-continuum(or [OII], or 158 [CII])FUV continuum ofmoderately massive starsneed SFH forinterpretation of SFRRegions with AV 1 hard tosampleExtinction correctionSFHfor lines line emissionf(n,T)Mid-IR continuumall luminosity heating ISMdustneeds extrapolation toFIR and SFH to get SFRPAH-strength?AGN contaminationEscape of UV-radiationMid-to-Far-IR SEDsSFHFar-IR continuumall luminosity heating ISMdustspatial resolution andsensitivity poor (butHerschel!)Needs SFH to get SFREscape of UV-radiationSFHRadio continuumsynchrotron emission FIR luminosity(FIR-radio relation)AGN contaminationUnclear physical originChanges with z & SFH ?
dependence on time & SF history (SFH)11111010Kroupa IMF, t 1e7 burst, solarKroupa IMF, continuous, solarK9810L(Lsun)/SFR(Msun/yr)101010K98 (LLyc 16 LH )910910881010LK-bandLFUVLLyc LH Lbol LFIR7107106106610710810age (years)9101010106107108109101010age (years)even the best star formation tracers are no better than 0.3dex, because ofuncertainties in in the underlying SFH and the assumed IMF. For extinctiondependent UV/optical estimators the situation is worse.
extinction : dependence on geometry‘screen’ : attenuation exp (- l)‘mixed’ : attenuation (1- exp (- l))/- lattenuation10.1near-IR, mixednear-IR, screenvisual, mixedvisual, screen0.010.1110100 lFoerster-Schreiber et al. 2000Rieke et al. 1993modified screen extinction estimators (Calzetti 2000) oftenare a reasonable description of the diffuse galactic extinctionbut fail in dense, dusty environments, where ‘mixed’extinctions are more appropriate
dust extinction2200 Ågraphite-featureN(H)/AV 1.8x1021 cm-2/mag(Bohlin et al. 1978)RV AV/E(B-V)MW: RV 3.1 (Schlegel et al. 2003)a dust model with a ‘Draine & Lee”mixture of graphites and silicatesgives a good description of Galacticextinction. The LMC/SMC andstarburst galaxies are betterdescribed by a greyer ‘Calzetti(2000) extinction curve’Draine 2003, astro-ph0304489V 0.556μmthe near- and mid-IR extinction toward the GalacticCenter & nearby starbursts is greyer than the Draine& Lee silicate/graphite dust model and requires thepresence of ices, increasing the 2-20µm dustabsorption (Lutz 1996, 1999, Fritz et al. 2011). Thefar infrared opacity (l) l , -1.5.-2 (Eales et al.2012, Scoville 2012, Magnelli et al. 2012)
mass tracersSimon Lilly lecture 1systematic uncertainties areparticularly hard to quantify andare often neglectedtracesissuesuncertaintiesUV to IR SED fittinglive stellar massrequires simultaneous fittingof M*, SFH, AVand assumption of IMFbest if rest-frame NIR coveredovercoming degeneracies,especially if z is unknown, oldstellar componentuncertainty 1.3-3rotating curvein Hα or COtotal dynamical massrequires spatially resolvedv(R) , fitting/info oninclination, deviations fromrotation? Mass outside brightregion sampled by lineemission?requires high SNR and 2kpcresolution with R 3000uncertainty 1.5-2velocity dispersionin absorption orCO/Hα emissiontotal dynamical massuncertain relation betweenrequires very longR1/2 and Rh,mintegrations for absorptionlinesrequires assumption on massdistribution in Runcertainty 2gas mass estimatorsdeviationhave uncertaintiesof 0.3 dex, becausefrom virialequilibriumunderlying SFH, IMFand extinction for the former, and forstellar, dynamical andof uncertainties in thegravitationallensing in spatialtotaldistribution,massonly possiblegalaxies in or factorsrequires r theaboutbehind clusters, or for chancemass distributionlatter.alignmentsuncertainty 1.5CO (HI) luminositymolecular (atomic) gas massrequires assumption onCO H2 conversion factorHI not accessible for high-zuntil SKAuncertainty 1.3- 3submillimeter dust luminositydust mass gas massrequires knowledge of Tdustand κdust( λ) andMgas/Mdustuncertainty 2
gas-star formation (Kennicutt-Schmidt)relation in z 0 star forming galaxiesXCO 2.3e20simple physical motivation: SFRN 1.4 0.2scatter 0.3 dex gas SFR hz ff gas 1/ 2 hz 1.5 hz gas hz 1/ 2 gas for cloudy medium a filling factor enters ingalactic averages, for marginally stable systems(Qtoomre 1) ff(local) dyn(galactic)Kennicutt 1998, Kennicutt & Evans 2012
classical papers star formation in nearby galaxieslate type galaxies formed over a longperiod of time with a Salpeter IMF, whiledwarfs show burstsnormal disk galaxies (SFGs) use up their gas reservoir ona time scale Gyr tHubble, requiring gas infall overcosmic time
spatially resolved SF- relation: THINGS/HERACLESBigiel et al. 200810 M pc 212 Spirals at 800 critpc ResolutionN 1HI H2HCNN 1in the regions where CO/HCN plausibly trace themolecular hydrogen content the average starformation is linearly correlated with molecular gasand dust, resulting in an approximately constantmolecular depletion time scale 1-2 Gyrs; it isunclear whether stars can form from atomic gas Little correlation between SFR and HI ΣHI saturates at 9 M pc-2Bigiel, Leroy, Schruba et al. 2008-2011, Gao & Solomon 2004
(specific) star formation rates dependsensitively on galaxy propertiesPre-SDSS: dependence on Hubble typeKennicutt 1998, ARAASDSS: dependence on concentration and surface densityKauffmann et al. 2003b
recent z 0 unbiased surveys of cold gas innormal star forming galaxies (SFGs)GASS/COLDGASS (PIG.Kaufmann) : stellar mass selection 1010 M ,0.025 z .05 fromSDSS/GALEX, 350 SFGsThere are sharp thresholds instructural parameters(especially stellar surfacedensity), above which thefraction of galaxies withdetectable HI or H2.decreasesstrongly. H2/HI and fmolgas areonly weakly correlated withgalaxy mass. High mass densitygalaxies are forming stars yetless efficiently, or have little gas.Catinella et al 2010, Schiminovich et al. 2010, Saintonge et al. 2011a,b, 2012, Kauffmann et al. 2012
star formation efficiency on galactic scalesM51 COM51 IRM51 QToomreIRAM COCARMA CO: Koda Spitzeret al. 2009near-IR-mid-IR (PAH) Hitschfeld et al. 2009star formationefficiency(1/depletion time) issimilar in/outsidespiral armsFoyle et al. 2010azimuththe KS relationbreaks down on 500pc scale, because oflocal evolutionaryeffectsSchruba et al. 2010,Onodera et al. 2010while molecular gas ispresent everywhere inthe disk, the mostluminous GMCs/dustyHII regions are locatedin the spiral arms andare associated withGiant MolecularAssociations ( 107.4M ); spiral arms areregions with Q 1where GMCs are‘formed’
discourse on observational capabilitiesfor galaxy evolution, from UV to radio
Key developments over the past 15 years(in terms of the experimental work) combination of efficient low noise, semi-conductor imaging detectors (e.g.CCDs, current record holder 2x109 pixels) & dedicated telescopes or largesurvey programs on the ground as well as in spaceSimon Lilly lecture 1W. Boyle & G. SmithNobel Prize Physics 2009J.GunnCrafoord Prize 2005
dedicated imaging surveyshttp://www.sdss.org/SDSS I-IIIPanSTARRSVISTA-VSTBigBOSSDESLSSTEUCLIDWFIRST Gunn et al. 1998
multi-band deep imaging surveys(UV to far-infrared)HDFGOODSCOSMOSCANDELS Spitzer, GALEX, Herschel follow-up
Large optical/infraredtelescopes2x10m Keck2x 6.5m Magellan Telescope8m GeminiNorth4 x 8m VLT10mHobby EberlyTelescope8m Subaru10m Gran Telescopio Canarias2x 8.2m Large Binocular Telescope
1990-2000 progress in large optical telescopes:light-weighting!Keck concept (Jerry Nelson): segmented mirror, with stresslapped hexagonal 1.8m mirrors which are co-aligned tobetter than 1/10 wavelength on starsVLT concept: thin meniscuszerodur mirror (Schott),supported by a large number ofactive optics pads (Wilson)LBT concept (Roger Angel):thin faceplate on stable,lightweighted honeycombceramic structure (borosilicate)Kavli Prize 2010 to Nelson, Wilson, Angelhttp://www.kavliprize.no/seksjon/vis.html?tid 45348
Concepts for 20m telescopesEuropean Extremely Large Telescope (42m)Giant Magellan Telescope(GMT 7x 8m telescope Super-LBT 22m)aplanatic Gregorian opticsThirty Meter Telescope (TMT CELT GSMT)five mirror, full adaptive, field stabilized design
Challenges for 20m telescopes reduction of current size-cost scaling by mass production ofsegments design and construction of large (adaptive) secondary/tertiary etc.optical mirrors achieving a reasonable and ‘instrument-friendly’ field-of-view( 5-10’) dynamic telescope control and field stabilization under realisticwind-shake conditions adaptive optics systems with large enough actuator density(several 103 elements) and bandwidth for realizing ‘D4’neardiffraction limited-science (especially 1.5μm) design and construction of (cryogenic) instruments, especiallywith significant field cost, especially also for operation ( 30-50 M /year)
HerschelJ W S Tamesebbpaceelescope 6m diameter telescope, self-deployable, assembled from 18 1.3m hexagon segments,passively cooled, L2, launch 2018? 4 instruments: NIRCAM, NIRSPEC, MIRI, FGS: 0.7-28 m, MOS, IFUpresentations: http://www.jwst.nasa.gov/publications.html,Gardner et al. 2007, Space Science Rev. (astro-ph0606175)10σ, 1Msec deep field, broad band sensitivity
Adaptive optics ‘Strehl ratio’ fraction ofenergy in centraldiffraction limitedspike: SR 1-Σj( Δj (rad) )Beckers 1993, Ann.Rev.A&Ap 31, 13wavefront sensordeformable mirrorfeedback with computerguide star(s)sensing/observing wavelength
laser guide stars in action at all majorlarge telescopes(Keck, Gemini, VLT)Keck/LLNL teamESO/MPE/MPIA teamGemini team
Multi-Conjugate Adaptive Optics forcorrection of a fieldbasic conceptstomography(first order: GLAO)From Ragazzoni 2000layer oriented /index.phpwide field AO (4’) 0.2-0.3”FWHM3 laser guide stars (x 2telescopes) GLAOpulsed green laser system(12 km altitude)Comissioning @ LBT in2013/2014
Large redshift surveys2dfVIMOSDEIMOSFMOS
Multi-object spectroscopy(multiplex 10-200)http://www.aao.gov.au/2dffiber positioner on AAT2d-F (AAT)FORS/VLT-multi-slitunit and spectra;upgrade to cryogenic near-IR MOSFIRE@Keckthe multi-ton DEIMOS,VIMOS, MOIRCS maskspectrographs atKeck/VLT/SUBARULUCIFER MOS html
Next generation: Prime FocusSpectrograph Subaruhttp://sumire.ipmu.jp/en/26522400 fibersacross 1.3 degree FOV
Multiplexed Near-IR spectroscopy:integral field spectroscopySPIFFI/SINFONI imageslicer30cm“3D”: Weitzel et al. 1994, 1996,“Tiger”: Bacon et al. 1995
KMOS: a glimpse into the future(most complex spectrograph ever built: 24 SINFONIs in one go!)‘fishermen @ pond’3 2kx2k RG HgCdTe Hawaii 2 detectors24 IFUs feeding 3 identical spectrographsperiscopeSharples, R. et al. 2006SPIE, 6269,E44, 2006 NewAR,50,370
Multi-object spectroscopy:JWST rd/news/topstory/2007/microshutters.html
Millimeter interferometry of cold gas:IRAM Plateau de Bure & NOEMANOEMA PdBIcurrentdoubling the collecting area: 6 12 telescopesRest wavelength [ m]11010010001000010Flux density10.10.010.0011.6 kmimproving resolution by factor 2 to 0.2”z 2.20.0001110100100010000Observed wavelength [ m]quadrupling bandwidth to 32 GHz
5000 m altiplano on ChajnantorALMAthe ultimatemm-interferometercurrently: 32 12m antennasfactor 10-30 improvement over current capabilities
Sensitivity of mm/submm-interferometryNOEMA goals - reach 33% ALMA line sensitivity& 50 % ALMA continuum sensitivity at 2-3mm1mm3mm- 2.3x sensitivity increase in the line& 4x sensitivity increase in the continuum over currentPdBISMA 20085mmCARMA 2008PDBI 2008NOEMAALMA
merging galaxy pair in local Universe: 106 M 'super' stars clusters with 104 O-stars NGC3603: massive star forming region in the Milky Way & local Universe: 104 M clusters with 100 O stars star clusters in galaxies 70-90% of star formation in the MW occurs in clusters (Lada & Lada 1993)
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On Galaxy Evolution Lane Challenge of measuring distances in universe Most striking: many galaxies experience collisions thus becoming "interacting galaxies . galaxy clusters NGC 4038/39 Antennae. 7 Birth of galaxies in clusters Few galaxies (none ?) BORN alone Collision of
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