Paul van der Werf

Leiden Observatory

HerCULES

Lorentz CentreFebruary 28,

2012

Introducing HerCULES

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Herschel Comprehensive (U)LIRGEmissionSurvey

Open Time Key Program on the Herschel satellite

HerCULES

Who is HerCULES?Paul van der Werf (Leiden; PI)Susanne Aalto (Onsala)Lee Armus (Spitzer SC)Vassilis Charmandaris (Crete)Kalliopi Dasyra (CEA)Aaron Evans (Charlottesville)Jackie Fischer (NRL)Yu Gao (Purple Mountain)Eduardo González-Alfonso (Henares)Thomas Greve (Copenhagen)Rolf Güsten (MPIfR)Andy Harris (U Maryland)Chris Henkel (MPIfR)Kate Isaak (ESA)Frank Israel (Leiden)Carsten Kramer (IRAM)Edo Loenen (Leiden)Steve Lord (NASA Herschel SC)

Jesus Martín-Pintado (Madrid)Joe Mazzarella (IPAC)Rowin Meijerink (Leiden)David Naylor (Lethbridge)Padelis Papadopoulos (Bonn)Dave Sanders (U Hawaii)Giorgio Savini (Cardiff/UCL)Howard Smith (CfA)Marco Spaans (Groningen)Luigi Spinoglio (Rome)Gordon Stacey (Cornell)Sylvain Veilleux (U Maryland)Cat Vlahakis (Leiden/Santiago)Fabian Walter (MPIA)Axel Weiß (MPIfR)Martina Wiedner (Paris)Manolis Xilouris (Athens)

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Conditions in ULIRGs Starbursts cannot be simply scaled up. More intense starbursts are also more efficient with their fuel. (Gao & Solomon 2001)

LIR SFR

LIR/LCO

SFR/MH2

SFE

1

1

1

1

1

H

400 :KL- BNOrion

54 :1-OMC

8.1 :GMCs Galactic

5.1 :WayMilky

100 :ULIRGs2

FIR

ML

ML

ML

ML

MLML

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(U)LIRGs (LIR>10(11)12 L)

(Evans et al.)

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(U)LIRGs from low to high z

LIRGs dominate cosmic star formation at high redshift

6HerCULES

(Magnelli et al. 2011)

ISM in luminous high-z galaxies

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Even in ALMA era, limited spatial resolution on high-z galaxies.

For unresolved galaxies, multi-line spectroscopy will be a key diagnostic

(Weiß et al. 2007)

HerCULES

(Danielson et al. 2010)

HerCULES in a nutshell HerCULES will uniformly and statistically measure

the neutral gas cooling lines in a flux-limited sample of 29 (U)LIRGs.

Sample: all IRAS RBGS ULIRGs with S60 > 12.19 Jy (6 sources) all IRAS RBGS LIRGs with S60 > 16.8 Jy (23 sources)

Observations: SPIRE/FTS full high-resolution scans: 200 to 670 m at R ≈ 600,

covering CO 4—3 to 13—12 and [CI] + any other bright lines PACS line scans of [CII] and both [OI] lines All targets observed to same (expected) S/N Extended sources observed at several positions

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HerCULES sampleTarget log(LIR/L)Mrk 231 12.51IRAS F17207—0014

12.39

IRAS 13120—5453

12.26

Arp 220 12.21Mrk 273 12.14IRAS F05189—2524

12.11

Arp 299 11.88NGC 6240 11.85IRAS F18293—3413

11.81

Arp 193 11.67IC 1623 11.65NGC 1614 11.60NGC 7469 11.59NGC 3256 11.56

Target log(LIR/L)IC 4687/4686 11.55NGC 2623 11.54NGC 34 11.44MCG+12—02—001

11.44

Mrk 331 11.41IRAS 13242—5713

11.34

NGC 7771 11.34Zw 049.057 11.27NGC 1068 11.27NGC 5135 11.17IRAS F11506—3851

11.10

NGC 4418 11.08NGC 2146 11.07NGC 7552 11.03NGC 1365 11.00

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Mrk231

HST/ACS(Evans et al., 2008)

At z=0.042, one of the closest QSOs (DL=192 Mpc)

With LIR = 41012 L , the most luminous ULIRG in the IRAS Revised bright Galaxy Sample

“Warm” infrared colours Star-forming disk (~500

pc radius) + absorbed X-ray nucleus

Face-on molecular disk, MH2 ~ 5109 M

HerCULES

Warning: may contain...

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quiescent molecular (and atomic) gas star-forming molecular gas (PDRs) AGN (X-ray) excited gas (XDRs) cosmic ray heated gas shocks mechanically (dissipation of turbulence) heated gas warm very obcured gas (hot cores)

HerCULES

Mrk231

SPIREFTS

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(Van der Werf et al., 2010)

HerCULES

Mrk231SPIREFTS

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Mrk231SPIREFTS

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Mrk231SPIREFTS

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Mrk231SPIREFTS

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Mrk231SPIREFTS

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Mrk231SPIREFTS

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CO excitation

2 PDRs + XDR 6.4:1:4.0

n=104.2, FX=28*

n=103.5, G0=102.0

n=105.0, G0=103.5

* 28 erg cm-2 s-1 G0=104.2

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CO excitation

3 PDRs 6.4:1:0.03

n=106.5, G0=105.0

n=103.5, G0=102.0

n=105.0, G0=103.5

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High-J lines: PDR or XDR? High-J CO lines can also be produced by PDR with n=106.5 cm—3 and G0=105, containing half the molecular

gas mass. Does this work?

G0=105 only out to 0.3 pc from O5 star; then we must have half of the molecular gas and dust in 0.7% of volume.

With G0=105, 50% of the dust mass would be at 170K, which is ruled out by the Spectral Energy Distribution

[OH+] and [H2O+] > 10—9 in dense gas requires efficient and penetrative source of ionization; PDR abundances factor 100—1000 lower

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Only XDR model works!

Analysis of analysis

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Model not unique At least 9 free parameters, not really a proper

fit Reasonable, based on prior knowledge External constraints available for all 3

components

... but what if we did not have this prior knowledge? role of H2O role of shocks role of OH+

Modeling-free result

Highly excited CO ladders are found in all high luminosity/compact sources with an energetically dominant AGN (and only in those sources).

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Water in molecular clouds

H2O ice abundant in molecular clouds

Can be released into the gas phase by UV photons, X-rays, cosmic rays, shocks,...

Can be formed directly in the gas phase in warm molecular gas

Abundant, many strong transitions expected to be major coolant of warm, dense molecular gas

24HerCULESHerschel image of (part of) the Rosetta Molecular Cloud

H2O in HerCULESTarget log(LIR/L)Mrk 231 12.51IRAS F17207—0014

12.39

IRAS 13120—5453

12.26

Arp 220 12.21Mrk 273 12.14IRAS F05189—2524

12.11

Arp 299 11.88NGC 6240 11.85IRAS F18293—3413

11.81

Arp 193 11.67IC 1623 11.65NGC 1614 11.60NGC 7469 11.59NGC 3256 11.56

Target log(LIR/L)IC 4687/4686 11.55NGC 2623 11.54NGC 34 11.44MCG+12—02—001

11.44

Mrk 331 11.41IRAS 13242—5713

11.34

NGC 7771 11.34Zw 049.057 11.27NGC 5135 11.17IRAS F11506—3851

11.10

NGC 4418 11.08NGC 2146 11.07NGC 7552 11.03NGC 1365 11.00 25HerCULES red = wet

H2O lines in Mrk231 Low lines: pumping

by cool component + some collisional excitation

High lines: pumping by warm component

Radiative pumping dominates and reveals an infrared-opaque (100m ~ 1) disk.

(González-Alfonso et al., 2010) 26HerCULES

Lessons from H2O (1 + 2 + 3 + 4)

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1) In spite of high luminosities, H2O lines are unimportant

for cooling the warm molecular gas. 2) Radiatively H2O lines reveal extended infrared-

opaque circumnuclear gas disks.

3) Extinction and radiative pumping of highest CO lines.

4) Detection of H2O lines implies high FIR radiation field, but not the presence of an AGN.

Lessons from H2O (5)

Radiation pressure from the strong IR radiation field:

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cTP /4d100rad

Since both 100 and Td are high, radiation pressure dominates the gasdynamics in the circumnuclear disk.

5) Conditions in the circumnuclear molecular disk are Eddington-limited.

Mechanical feedback Radiation pressure can drive

the observed molecular outflows (e.g., Murray et al., 2005)

Aalto et al., 2012: flow prominent in HCN dense gas

Key process in linking ULIRGs and QSOs?

Shocks probably of minor importance in Mrk231

29HerCULES (Feruglio et al., 2010)

(Fischer et al., 2010)

NGC6240: CO lines as tracers of what?

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X-ray nuclei AGNs?

PAH emission PDRs?

H2 lines shocks!

NB: FTS shows 12CO/13CO > 50 ! Optically thin CO lines

NGC253: shocks or PDRs?

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chemistry shocks?

H2 lines PDRs!

SINFONI H2 v=10 S(1), Rosenberg et al., in prep.

NGC7469

SPIREFTS:

CO ladder

suggests PDR?

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NGC7469SPIREFTS:

OH+ suggests

XDR?

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NGC7469SPIREFTS:

OH+ suggests

XDR?But no H2O+...

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High-z connection (1): H2O at z=3.9

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Line ratios similar to Mrk231 FIR pumping dominates, implies 100 m-opaque disk Radiation pressure dominates, Eddington-limited

Van der Werf et al., 2011