Download - HerCULES
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Paul van der Werf
Leiden Observatory
HerCULES
Lorentz CentreFebruary 28,
2012
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Introducing HerCULES
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Herschel Comprehensive (U)LIRGEmissionSurvey
Open Time Key Program on the Herschel satellite
HerCULES
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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
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(Magnelli et al. 2011)
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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)
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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
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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)
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Mrk231
SPIREFTS
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(Van der Werf et al., 2010)
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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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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!
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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+
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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
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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
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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
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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.
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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.
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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)
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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
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NGC253: shocks or PDRs?
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chemistry shocks?
H2 lines PDRs!
SINFONI H2 v=10 S(1), Rosenberg et al., in prep.
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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