HERSCHEL and Galaxies/AGN “dust and gas”. Peter Barthel Kapteyn Inst. Groningen, and Herschel Science Team. 1. Masses of spheroidal components in galaxies grow with their central black holes. THE issues. (from Luis Ho). (SDSS, from Kauffmann et al.).
HERSCHEL and Galaxies/AGN“dust and gas” Peter Barthel Kapteyn Inst. Groningen, and Herschel Science Team
1. Masses of spheroidal components in galaxies grow with their central black holes THE issues (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 2 1 log [n(z) / n(peak)] log [d* /dt/M yr-1 Mpc-3] 0 -1 (Madau & Pozzetti 2000) 3. SFR(z), nQSO(z) and the nature of submm galaxies Z Z
Furthermore: • Bulges in place within a Gyr after the Big Bang • Massive BHs accreting processed material • Molecular gas ubiquitous (SDSS, from Fan et al.)
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
HERSCHEL will be an SED-machine HST: NGC7742
log(S 60 / S20cm) = u =2.03 Note extra-strength FIR, correlating with synchrotron radio
Spoon (PhD thesis) Note the increasing MIR/FIR effects of star-formation
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)
(van Bemmel) Cold, warm and hot dust in the host of Cyg A
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.
HERSCHEL will extend our understanding of the star-formation efficiency in galaxies(together with ALMA!)
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 BCDs Dust in ellipticals Effects of bars, mergers Cluster effects SFRs: 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!