Imaging the IGM/CGM. Christopher Martin California Institute of Technology For CWI, KCWI, FIREBALL,ISTOS Teams. IGM Matters Heidelberg June 2014

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1 Imaging the IGM/CGM Christopher Martin California Institute of Technology For CWI, KCWI, FIREBALL,ISTOS Teams IGM Matters Heidelberg June 214

2 1. IGM tracing structure interconnecting galaxies Agertz, Teyssier, Moore 29 5 pkpc 3. Galaxy properties depend on recent gas flow (in/out) 4. Star forming galaxies fed by cold streams from Cosmic Web 2. Most baryons in IGM, Some in warm IGM 5. Star forming galaxies are ejecting gas & chemicals into Cosmic Web

3 Why Emission? Scale θ Size L = θd Mass M Overdensity δ Density n i = N i /L Ionization Γ/n Total density n = f(γ, n i ) Pressure p=nkt Filling Factor f Temperature T pressure Heating/cooling balance Timescales cooling t cool ~ T/nL Collapse time t ~ δ -1/2 Morphology outflows/inflows shocks, filaments Gas Kinematics Divergence Rotation Correlation of IGM w/ galaxies, AGN - Circum-galactic medium - Gas reservoirs - Inflow, accretion - Outflow, feedback Large Scale Structure Mapping large scale structure statistics P(k) v v r δ k phases (non-gaussian?)

4 Distance 11,354 Million Lt-yr Redshift 3. Wavelength 4864Å Distance 11,362 Million Lt-yr Redshift 3.1 Wavelength 4876Å Distance 11,37 Million Lt-yr Redshift 3.2 Wavelength 4888Å Map IGM/CGM using 2D Imaging Spectroscopy of Rest UV Lines: Ly, CIV, OVI

5 Observational Strategies Enabled by 2D Imaging Spectroscopy of Rest UV IGM/CGM Emission 1) Direct Detection à Maximize deep exposure volume à Optimal smoothing on extended scales 2) Stacking on known galaxies à redshift survey regions à large survey volume 3) Stacking on galaxy-traced filaments à redshift survey regions à low luminosity galaxies 4) Cross-correlate QSO abs/igm em à redshift survey regions à low luminosity galaxies 5) Cross-correlate Gal abs/igm em à redshift survey regions Lyman alpha Fluorescence (Cantalupo et al 25)

6 IGM Project Imaging & Mapping the Hidden Cosmic Web of Baryons ISTOS Explorer Å.5<z Lyα <1.2 FIREBALL Balloon Å.7<z Lyα <.85 KCWI Keck 35-1,5Å 2.<z Lyα <7.2 Time since Big Bang Billion yrs Goals (rough chronological order) Redshift (1) Discover & map Circum-Galactic Medium (CGM) & IGM-galaxy co-evolution ISTOS... F KCWI-B KCWI-R (2) Discover & map IGM emission from the hidden baryons (WHIM, cosmic web) Cosmic Epoch WHIM Grows, SF dies Star Formation Epoch SF Grows Reionization (3) Use IGM emission to trace large scale structure & cosmology (4) Detect & map emission from growing reionization HII regions Wavelength (µm)

7 FIREBALL Faint Intergalactic Redshifted Emission BALLoon Detecting the Circum-Galactic Medium at low redshift Caltech, JPL (Nikzad), LAM (Milliard), Columbia (Schiminovich), CNES Goals 1 Discover & map Circum-galactic medium to explore IGM-galaxy co-evolution 2 First demonstration of high QE UV photon-counting detectors and UV IFS and MOS

8 Targeting CGM Regions

9 ISTOS Imaging Spectroscopic Telescope for Origins Surveys Revealing the Hidden Cosmic Web of Baryons Caltech, JPL (Nikzad), LAM (Milliard), Columbia (Schiminovich), + Goals 1 Discover & map IGM emission from the hidden baryons in the Universe 2 Discover & map Circum-galactic medium to explore IGM-galaxy co-evolution 3 Decode the star formation laws at low and high redshift 4 Explore the extended, low surface brightness UV Universe

10 CWI Cosmic Web Imager Chris Mar1n, Anna Moore, Ma5 Ma5euzski, Patrick Morrissey, Daphne Chang, Shahin Rahman 3D, Low Surface Brightness Spectroscopy at Palomar Science Applica+ons (examples) 1 Map circum- galac1c medium 2<z<7 2 Map circum- QSO medium 3 Composi1on & age of stellar remnants (halos, intracluster light) 4 Low mass/surface brightn. universe 5 Galaxy kinematics & stellar pops 6 GRB/SNe host properties 7 Galactic superwinds/feedback Design ü Integral Field Spectrograph: 6 x 4 arcsec 2 ü R~5 spectrograph ü 1 channel, μm coverage w/ mul1ple gra1ngs ü Designed for low surface brightness emission ü Designed for precision sky subtrac1on ü First light 29

11 CWI : Image Slicer 6/17/11 11

12 S B Nod & Shuffle see Sembach and Tonry 1996

13 Comparison of Sky-Sky Test with Sky-Background e/12 s e/12 s Sky Sky Pixel Src Sky Pixel

14 Nod-and-Shuffle Frame Source Sky Source-Sky

15 CWI: Gas Flows in Galaxies Gas Flows that Trigger Star Formation Turbulent Gas the Regulates Star Formation? HβMosaic Image HβVelocity Map HβVelocity Dispersion Map M51 Whirlpool Galaxy v(residual) [km/s] σ v [km/s]

16 CWI: Gas Flows in Galactic Halos CWI Light bucket spectroscopy of NGC891 halo [OIII] Hβ

17 CWI: Diagnosing Stellar Halos CWI Light bucket spectroscopy of NGC891 stellar halo

18 CWI: Gas Flows to Circumgalactic Medium GALEX NUV M82 Superwind Outermost Shell CWI [NII] H [NII] [NII] H [NII] 2 1 [NII] H [NII]

19 Circum-QSO Medium

20 Palomar CWI Inflow from Cosmic Web Filament to Quasar Caltech Press Release April 28 Results from Palomar Cosmic Web Imager Martin et al. 214a

21 Distance 11,354 Million Lt-yr Redshift 3. Wavelength 4864Å Distance 11,362 Million Lt-yr Redshift 3.1 Wavelength 4876Å Distance 11,37 Million Lt-yr Redshift 3.2 Wavelength 4888Å q l

22 CWI: Circum-QSO Medium Lyα emission near QSO [arcsec] [Å] 4669Å 22

23 CWI: Circum-QSO Medium Lyα emission near QSO Å

24 CWI: Circum-QSO Medium Lyα emission near QSO [arcsec] [Å] 4669Å 24

25 Lyα emission from IGM Cosmic Web 3 Million Lt-yrs 3 Million Lt-yrs 25

26 4 Caltech Press Release April 28 Results from Palomar Cosmic Web Imager Martin et al. 214b, ApJ, April 2.

27 4 L(Fil) L(Blob) Intensity Velocity Caltech Press Release April 28 Results from Palomar Cosmic Web Imager Martin et al. 214b, April 2.

28 4) How does gas get into galaxies? Cold Flows à Forming/Refueling Galaxies L[Lyα] ~.8 L[grav]? M DM = M M DM = M Rosdahl and Blaizot 212

29 Emission Models Spectral Image Plots 5 pkpc Cantalupo+5

30 Spectral-Image Plot Lya emission simulation Cantalupo Million Light-years

31 CGM Emission & Kinematics z~3 Lyman α blob Emission Spectral Image 4669Å 31

32 CGM Emission & Kinematics z~3 Lyman α blob Emission Spectral Image 4669Å 32

33 Extended Cold-flow Disks produced by cold accretion from IGM Stewart+213 Velocity Profile

34 IGM/CGM Emission & Kinematics z~3 Lyman α blob is an extended, warped protodisk with inflow from filaments? Inner Disk Outer Disk/Ring 1 kpc Inflow from Cosmic Web 4669Å Martin+213, CWI IGM Paper III, in prep..

35 IGM/CGM Emission & Kinematics Kinematic profile at 45 DATA R45 MODEL R [Å] [Å] Martin+213, CWI IGM Paper III, in prep..

36 IGM/CGM Emission & Kinematics Kinematic Profile at 2 DATA R MODEL R [Å] [Å] Martin+213, CWI IGM Paper III, in prep..

37 Lyman α Emission Profile Physical Diagnostics à N HI, σ, Δv w = f(n HI,σ,Δv) p = g(n HI ) = Δλ/w t = h(δv) = I + - I - I + + I - p=δλ/w t = w λ λ w λ t =.5 w λ w λ w λ

38 HeII 164Å vs. Ly alpha 1216Å Galaxy Formation & Gravitational Cooling HI 1216 HeII 164 Yang+6

39 4) How do galaxies get their gas? What is the role of hot vs. cold accretion over mass and time? log ρ ρ = log δ ( ) Cold Mode Hot Mode Cold Mode Accretion log( T[K] ) Birnboim & Dekel 23; Keres+24; Dekel & Birnboim 6, 8; Dekel+ 29

40 KCWI Flexible & Powerful 2D Spectroscopy DSS Stephan s Quintet 24 Slitlet spectra PCWI λ KCWI 3 selectable image slicers! Hβ Continuum Slicer Field of View Spatial Resolution Spectral Resolution Small 2 x 8.6 x Å (R 2,) Medium 2 x 16.6 x.7.45 Å (R 1,) Large 2 x 32.6 x Å (R 5,)

41 KCWI Keck Cosmic Web Imager 3D, Low Surface Brightness Spectroscopy at Keck Key Features Wide spectral range (35-15Å) Flexible field of view, image resolution Flexible spectral resolution, coverage Superb sky subtraction Excellent imaging & Dark Sky on Mauna Kea 1 st Light Spring 215 (KCWI-Blue) Science Applications (examples) Map circum-galactic medium 2<z<7 Map circum-qso medium Map z~6 reionization bubbles Composition & age of stellar remnants Unusual stellar nebulae Low mass galaxies Galaxy outskirts Galaxy kinematics & stellar age, composition Galaxy gas halos, fountains Stong lens systems Transient sky -- Explosions Galactic superwinds/feedback Exoplanet transit spectroscopy

42 Keck Cosmic Web Imager Team Steve Kaye Randy Bartos Patrick Morrissey CM Anna Moore Don Neill Sean Adkins Connie Rockosi Connie Rockosi Drew Phillips Drew Phillips Jason Fucik Bob Weber Alex Delacroix Matt Matuszewski Harland Epps Harland Epps Sean Adkins Valerie Duval Mike Kokorowski Matt Matuszewski 42

43 CWI/FIREBALL/ISTOS New tools for mapping IGM/CGM KCWI Keck 35-1,5Å 2.<z Lyα <7.2 Summary Evidence for Filamentary Extensions and Inflow into QSO Extended Filamentary Emission around LAB Strong HeII Emission 2 I[LU]