HERSCHEL and Galaxies/AGN
“dust and gas”
Peter Barthel
Kapteyn Inst. Groningen,
and Herschel Science Team
THE issues
1. Masses of spheroidal components in galaxies grow with their central black holes
(from Luis Ho)
(SDSS, from Kauffmann et al.)
2. Nuclear accretion and circumnuclear star-formation are astrophysically connected processes
Quasar space density Star formation rate
(Madau & Pozzetti 2000)
log
[dlo
g [d
* * /d
t/d
t // M
M
yryr
-1-1 M
pc M
pc-3-3]]
log
[n(z
) /
n(pe
ak)]
log
[n(z
) /
n(pe
ak)]
3. SFR(z), nQSO(z) and the nature of submm galaxies
Z Z
0
-1
1
2
(SDSS, from Fan et al.)
Furthermore:4. Bulges in place
within a Gyr after the Big Bang
5. Massive BHs accreting processed material
6. Molecular gas ubiquitous
In other words:
star-formation and nuclear activity MUST go hand-in-hand in some way, throughout the history of the Universe
NGC1068
HERSCHEL SPACE OBSERVATORYvs. Galaxies/AGN -
what achievements can we foresee?*
*however, recall that many achievements cannot be foreseen!
So where IRAS opened the dusty and molecular Universe …..
….ISO and Spitzer have subsequently carried out detailed studies
ISO and Spitzer observe(d) processes at MIR/FIR wavelengths, with emphasis on star-formation and other mechanisms affecting dust and gas in galaxies:
MIR/FIR colors, luminosities, temperatures MIR aromatic features MIR/FIR diagnostic lines, cooling lines line/continuum ratios ………..
HERSCHEL will continue where the previous missions stopped
extending -range into submm at much greater sensitivity, higher spatial resolution, and spectral resolution
This will permit studying the MIR/FIR out to extreme redshifts
HST: NGC7742
HERSCHEL will be an SED-machineSED-machine
Note extra-strength FIR, correlating with synchrotron radio
NGC 7742
-2
-1.5
-1
-0.5
0
0.5
1
-1 0 1 2 3 4 5 6
log wavelength (micron)
log
flu
x d
en
sit
y (
mJ
y)
log(S 60 / S20cm) = u =2.03
Note the increasing MIR/FIR effects of star-formation
Spoon (P
hD thesis)
HERSCHEL will adress the symbiosis of MBH accretion activity and star-formation out to high z, using spectroscopic observations, as well as:
(ISO work by Lutz, Genzel & Co.)
… analysis of the global FIR SEDs, taking multicomponent dust models into account
(from Sanders)
Cold, warm and hot dust in the host of Cyg A
(van Bem
mel)
Radio galaxies with, and without recent star-formation (FIR SED!)
HERSCHEL will measure global FIR SEDs out to extreme redshifts, for many classes of objects
Measuring the full dust SED, Herschel will be the ideal tool to investigate (obscuring) dust in distant AGN, radio-loud as well as radio-quiet.
The relative and absolute importance of obscured (Type-2) AGN can be addressed.
Mature, quiescent ellipticals?
HERSCHEL will extend our understanding of the star-formation efficiency in galaxies(together with ALMA!)
CO detected PG QSOs
10.00
10.50
11.00
11.50
12.00
12.50
9.00 9.20 9.40 9.60 9.80 10.00
log M(H2)
log
L(F
IR)
PG QSOs (z<0.05) PG 1700+518
The spectroscopic diagnostics will be used, also at high redshift
(from Genzel et al.)
Together with ALMA and radio arrays (incl. LOFAR) the radio-FIR correlation can be employed out to extreme redshifts
(from Condon and Broderick)
Details of the radio-FIR correlation can be investigated
Spitzer: q-distribution
The physics, kinematics and energetics of the star-formation process and relevant radiative transfer processes (incl. cooling) will be studied, employing 1D and 2D spectroscopy.
Template spectra will be obtained, in a variety of objects/conditions
(Spitzer IRAC)
Galaxies in the local Universe will be surveyed, adressing:Dust and gas in BCDsDust in ellipticalsEffects of bars, mergersCluster effectsSFRs: photometric end spectral line mapping ……………….
! The resulting SED and line templates will be used at all redshifts
In summary, Herschel will deal with star and galaxy formation, globally and in detail:
MW, PDRs, GMCs, SSCs, BCDs, Es, LBGs, EROs, DRGs, SMGs, QSOs, RGs, CSSs, ULIRGs, ….., you name it!
We live in exciting times and Herschel is going to make it even more exciting – feel free to join the fun/excitement!
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