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What matter(s) around galaxies? Shining a bright light on the cold phase of the CGM Cantalupo et al., Nature , 2014 Sebastiano Cantalupo ETH Zurich In collaboration with: MUSE GTO Team (ETH, CRAL, Leiden, AIP, Toulouse, Gottingen) + Cosmic

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Sebastiano Cantalupo – What Matter(s) Around Galaxies - June 2017

What matter(s) around galaxies? Shining a bright light on the cold phase of the CGM

Sebastiano Cantalupo

Cantalupo et al., Nature, 2014

ETH Zurich

In collaboration with:

MUSE GTO Team (ETH, CRAL, Leiden, AIP, Toulouse, Gottingen) + Cosmic Structure Formation group at ETH & J. Xavier Prochaska, Sammy B. Slug, Piero Madau, Fabrizio Arrigoni-Battaia, Joe Hennawi , Martin Haehnelt

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Cantalupo et al., Nature, 2014

Talk Outline & Key Questions

What are the morphological and physical properties of the CGM on both small and large scales? (key questions #2 and #3) How do galaxies affect cooling in the CGM? (key question #4)

Observational surveys (NB, MUSE, MOSFIRE) and inferred properties of the CGM

Open questions/Summary

Introduction: detecting the CGM/IGM in emission

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Direct detection in emission: Fluorescent Lyα (Hogan & Weymann 1987;Gould & Weinberg

1996; Zheng & Miralda-Escude 2005; Cantalupo+05,07; Kollmeier+06,10; Cantalupo+12)

external ionizing flux HI ionized region

(HII)

fluorescent emission

HII recombina- tions

HI

Absorption part (1D info)

fluorescent emitters QSO

Self-shielded gas (slab): “mirror” emission -> ~60% of incident ionizing radiation “converted” to Lyα (but see Cantalupo+05). Fully ionized gas: proportional to gas density squared.

Detecting Cosmic Gas

“Classical” approach: in absorption.

  • pro: ability to detect low-density gas including metals.
  • con: typically only 1D information (or sparse 2D)

LLS/DLAS = “Dark” galaxies? Filaments? IGM? CGM? ... difficult to say without direct detection. quasar

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UVB+Stars UVB+Stars +QSO

UVB fluorescence

QSO fluorescence

log(SB) (cgs/arcsec2)

Simulated Lyα images at z~2.5 (20Å NB; no noise/PSF) centred on a ~1013 Msun halo hydro-simulation (RAMSES) + Radiative Transfer (RADAMESH, SC+12)

Cantalupo+12

How bright is fluorescent emission: simulations

NB & MUSE 1h MUSE medium MUSE deep

  • 17
  • 18
  • 19
  • 20
  • 21

2 4 6 8 cMpc 2 4 6 8 cMpc MUSE FOV

1) Look around bright quasars 2) “Stack” for statistical detection (see Sofia Gallego’s talk) 3) Integrate for 100+ hours away from quasars How to detect it?

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Highlights from Narrow-Band imaging survey of Quasar fields at z~2.3

Compact fluorescent emitters without stellar counterparts (“Dark galaxies”) SC+12

1’ (500kpc)

Giant Quasar Nebulae: the Slug

Cantalupo+14, Nature qso

CGM in emission around a bright galaxy

Morphology and SB compatible with “cold filaments”

SC+12

qso (3’)

+other 25 QSOs (FLASHLIGHT Keck+GMOS survey;

Cantalupo+, in prep.; Arrigoni-Battaia+, in prep.; see next talk) main results:

  • Giant Nebulae (>100kpc) are rare in NB surveys (<10%)
  • Morphology and “kinematics” compatible with

CGM/IGM but SB is too high for expected gas densities —> dense clumps required (see later).

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45” ~350 kpc

“White-light” images

  • btained by collapsing

the datacube along the wavelength direction. Borisova, Cantalupo+, 2016 Exposure times: 1h only total integration (“snapshot” survey) Targets: brightest radio-quiet QSOs at 3<z<4 (and two radio-loud, R1 & R2)

Are Giant Nebulae really rare? A MUSE snapshot survey around z~3.5 QSOs

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45” ~350 kpc

Optimally extracted pseudo-NB images with QSO PSF-subtraction

  • btained with CubExactor

(Cantalupo in prep.) Borisova, Cantalupo+, 2016 All nebulae larger than 100 kpc with various morphologies.

MUSE observations of QSOs at z~3.5: 100% detection rate of giant nebulae!

Exposure times: 1h only total integration (“snapshot” survey) Targets: brightest radio-quiet QSOs at 3<z<4 (and two radio-loud, R1 & R2)

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A 3D view of the Muse Quasar Nebula 3 (MQN03), 350kpc in size:

CubExtractor (Cantalupo, in prep.) + VisIt QSO PSF and continuum subtracted cube

Borisova, Cantalupo+, 2016

2σ~1x10-18 cgs/arcsec2 10A ~ 600km/s

350kpc

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2D Velocity maps:

  • no clear signs of “rotation” (with some exceptions);
  • radio-quiet nebulae (1-17) are kinematically “narrow”.

Borisova, Cantalupo+, 2016

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How do they compare with other Lyα Nebulae and “haloes”?

Circularly averaged SB profile

All giant quasar nebulae have similar SB profile and are consistent with fluorescence (including LBG Stack “halo” of Steidel+11)

average profile

Borisova, Cantalupo+, 2016

“redshift-corrected” (all scaled to z=3)

QSO PSF

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M(HI) ~ M(“cold” H) ~ 2.5x1011 M⊙◉☊

“Photon-pumping / Lyα scattering” case (gas mostly neutral)

Inferred N(HI)

M(HII) ~ M(“cold” H) ~ 1012 M⊙◉☊/C0.5

Inferring the cold gas content of the Giant Nebulae: the Slug case Inferred N(HII) Observed SB

“Recombination” case (gas mostly ionized)

cm-2 cm-2

a a b b

Cantalupo+, Nature, 2014

NB: depends on Clumping Factor

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Comparison with simulations: more IGM “clumps” needed! Simulation (all) “neutral” case “ionized” case “ionized” case C=1 C=50

N(H) cm-2 N(H) cm-2

Slug Nebula Slug Nebula Slug Nebula Text

a a a b b b

Cantalupo+, Nature, 2014

Subgrid Clumping Factor (<1kpc) Subgrid Clumping Factor (<1kpc)

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Breaking degeneracies with non-resonant lines: MUSE HeII search NB (Ly𝛃)

c

Cantalupo+, in prep.

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continuum subtracted cube (9h) + CubEx v1.6 (Cantalupo, in prep.)

Extended HeII detected with MUSE from “part” of the Slug (no rotation!):

Cantalupo+, in prep.

c

12 6 4 2

2σ~3x10-19 cgs/arcsec2 10A ~ 600km/s

150kpc

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Why is HeII “missing” from the Slug “tail”? “tail” Lyα spectrum

Leibler, Cantalupo+, to be sumbitted

Hα spectrum “tail”

qso b

1) “Tail” Lyα emission due to “photon-pumping / scattering” ruled out by MOSFIRE Hα (and preliminary MUSE CIII) detection

Lyα/Hα~10

consistent with Case B Recombination

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HeII/Lyα

~0.08 <0.005!

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“single-density” clump scenario

(a)

  • 3.5
  • 3
  • 2.5
  • 2
  • 1.5
  • 1
  • 0.5
  • 1

1 2 3 4 log (HeII/Lyα) log(nH/cm-3) Expected HeII/Lyα ratio D = 50 kpc D = 160 kpc D = 350 kpc D = 1 Mpc

data

(a)

nclump~102 -104 cc ! (depending on actual distance)

(b)

“turbulent/lognormal density distribution” scenario

<n>cold=1 cc <n>cold=0.1 cc

data data

(b)

<n>cold ~1-10 cc if log-normal σ >2.5

Cantalupo+, in prep.

2) High densities and larger distances

Why is HeII “missing” from the Slug “tail”? High densities required

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Open Questions and Future Directions

What sets the frequency, size and luminosity of the giant quasar Nebulae? (quasar lifetime, opening angle, halo mass, redshift, quasar luminosity,…) What is the origin of the IGM/CGM clumps traced by the Nebulae? (thermal/gravitational instabilities, quasar radiation effects,…) How this affects galaxy and QSO formation? (fast gas accretion, violent disk instability,…)

Exploring a larger parameter space:

  • include lower luminosity quasars;
  • extend the redshift range to 2<z<3 (not possible with MUSE, KWCI required)

Improving our theoretical understanding of IGM “clump-formation”:

  • hydrodynamical and thermal stability analysis (see Ann-Christine Vossberg’s talk);
  • detailed comparison with observational data.

Moving “away” from quasars:

  • detect “average” Cosmic Web filaments connecting galaxies and illuminated by the

cosmic UVB (>50h-deep exposure with MUSE and/or KWCI required).

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“We understand everything about gas cooling [in the CGM] thanks to our hydrodynamical simulations, so we only need to focus on SN and AGN feedback.”

A Colloquium Speaker, IoA, Cambridge, 2009

1) removing the gas from the galaxy (e.g., SN feedback, “ejective feedback”). 2) reducing/stopping cooling gas accretion from the CGM by “changing” cooling ion abundances (“preventive feedback”)

What happens when the CGM is “illuminated” or how to “quench/regulate” the SFR of galaxies? The basics of the Cooling Function

cooling function with UVB

Main coolants: ion line Ion.Potential O4+ OV[630A] 113.9 eV Ne5+ NeVI[400A] 157.9 eV Fe8+ FeIX[169A] 233.6 eV

To “kill” the peak cooling rate we need to “illuminate” the CGM with soft X-ray photons

Wiersma+2009

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Strickland+04

Soft X-ray emission from GALAXIES: linear relation with SFR

See also: Mineo+15

Rovilos+09

Soft X-ray (model) produced by SN bubbles, calibrated to reproduce observed SFR - Soft Xray relation. NB: X-ray binaries not included(yet)

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Effect on the CGM cooling: Cloudy modeling for “typical” CGM

cooling heating nH=10-3 cm-3 (δ~5x103 @ z=0) (δ~6x102 @ z=1) d=5 kpc from galaxy Z=0.03 Z⊙ Λ(n, T, Z, U*+UUVB) U*∝ SFR × d-2 × nH-1 NB: for isothermal halo profile: U*∝ SFR × Mvir-2/3 × (1+z)-1 dramatic effect of local sources on cooling rates

  • f CGM gas (+ some extra

heating).

Cantalupo 2010

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Result: transition depends on SFR. For high SFR there is no “critical halo mass”.

Cantalupo 2010

The hot-mode/cold-mode transition (Dekel & Birnboim 2006) revisited

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Importance of this effect is confirmed by hydrodynamical simulations

Kannan,…,Cantalupo+2014

CGM CGM

“standard”

+ local X-ray

+ local X-ray

“standard”

ISM ISM

  • Gasoline simulations (isolated disk)
  • SFR and total stellar Mass reduced by a factor of 2
  • SFR “regulated” when critical SFR is

reached (as in analytical model)

  • Less SN feedback “required”,

improved rotation curve, more stable disk.

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Observational evidence for local source effect on CGM cooling?

Tumlinson+11

  • “absence” of the main cooling line (OV630A) is difficult to probe directly.
  • indirect evidence: excess of O5+ (OVI) or higher potential ions.

COS-Halo Survey

Werk, Prochaska, Cantalupo+16

Oppenheimer+16 (EAGLE zoom simulations) data (points)

simulations (lines)

  • clear excess of OVI close to star forming

galaxies w.r.t. simulations without local radiation effect (e.g. Oppenheimer+16)

See Jess Werk’s talk and others on Thursday

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Summary and open questions

New technique to “illuminate” the CGM/IGM at high-z with the help of QSOs: Giant Lyα Nebulae with sizes up to 500kpc and various morphologies are ubiquitous around QSOs at z~3.5 (MUSE) and apparently less frequent in NB surveys at z~2. (key question #2).

Is this a real redshift evolution or due to the observational technique?

Modelling of both H-Lyα and HeII emission suggest that clumps with large densities (n>>10 cm-3) and small sizes (~pc) or log-normal/turbulent density distributions with large σ should be present on intergalactic scales around quasars. (key question #3) What is the origin of the clumps and their effect on galaxy formation and evolution? Local sources of X-ray radiation can greatly reduce CGM cooling (increasing NOVI) and therefore regulate star formation without the need of strong ejective feedback at z<1 (key question #4). How this affects galaxy properties such as, e.g. disk angular momentum?

Next future:

  • ultradeep MUSE surveys to trace largest filaments
  • new theoretical/numerical CGM models to resolve the

“small-scale” physics

Stay tuned!