Letters of Intent received in 2015

LoI 2017-299
SuperMassive Black Holes and star formation in the Universe

Topics

Supermassive Black Holes and star formation history in the Universe: A stellar population point of view
1. Star formation physics and star formation laws
2. Metals-dust models for AGN+ galaxies (radiative transfer, extinction laws)
3. Stellar Black Hole mass evolution by galaxy types
4. Supermassive Black Hole mass (models vs observations)
Comparison with SNRs
5. Luminosity and mass functions: Galaxy and AGN counts
6. The link with numerical simulations of galaxy formation
After Herschel+Spitzer, Keck+HST, Planck, ALMA+JVLA
Perspectives with JWST, EUCLID plus statistics tools and numerical simulations

Rationale

The two main objectives of this demand are to clarify the debated subjects on:
i) Super Massive Black Holes hosted in massive galaxies up to z>4: from SuperNova Remnant migration?
ii) the link of semi empirical models of Galaxy Evolution and numerical simulations of galaxy formation

For a further comparison with dynamics and numerical simulations, the evolutionary modeling of stellar populations is proposed in the present symposium in relation with the growth of supermassive black holes, inducing the AGN torus far-IR emission, scattering and polarization.
Focuses are on the birth, evolution and death of stars, dividing the stellar populations in two parts: i) luminous (including attenuated) star photospheres, nebular and dust emissions, all traced by the global SED ii) the already died population (SNRs and WD), all traced by chemical ejecta, stellar black holes and neutron stars and possibly white dwarfs when the galaxy is observed at the age t (redshift z). Relations of stellar masses, BH masses and their respective activities are analyzed.
Only specific conditions of star formation process allow to justify the migration of stellar black holes towards the galaxy core: size of star formation knots in relation with densities, velocities, metallicities and environmental properties. The following of galaxy evolution: intrinsic or passive due to internal stellar models and active from star formation laws (Starburst99, Pégase (1997, 2015), Bruzual &Charlot 2003, Maraston 2005, Cigale 2009) is then associated to numerical simulations to follow mergers or intercations, gravitation, taking into account dynamical friction modeling (Alexander, 2015). Interpretations of z=4 galaxies are presented with Pégase (Rocca-Volmerange et al., 2013, 2015).
Observations are continuous multi-wavelength SEDs suffering difficulties for a significant comparison of fluxes measured with low to high spectral resolutions or through various apertures (for example: to compare HST to Herschel data requires important corrections).
The modeling of AGNs (Fritz et al, 2006, Siebenmorgen 2014 and others) is in progress with far-IR, submm and mm data . Requiring to be related to bolometric AGN emission (UHE, X-rays and radio), the disentangling of AGN torus with recent or evolved star formation is being quantified (Drouart et al, 2015, submitted to A&A, Podigachoski et al., A&A, 575, 80).
By associating the star formation laws of massive galaxies and the modeling of AGN including constraints on star formation knots and laws by types, we derive the possibility to predict the number and mass densities of black holes along the star formation history of the Universe, based on mass and luminosity functions of AGN and Galaxies. Larger scales (galaxy groups, clusters and dense environments) are required to follow the galaxy populations at the highest z by counting their detections and magnitudes. The two domains are constrained by the modeling of galaxy evolution at large structure, using cosmostatistics (Wandelt et al., 2012) and the initial conditions adopted in numerical simulations (Dubois et al, 2014).
References
Alexander, T., arXiv, 50504823
Bruzual, G., Charlot, S., 2003, MNRAS, 344, 1000
Drouart, G., et al., 2014, A&A, 566, 53
Drouart, G., et al. 2015, submitted to A&A
Dubois et al., 2014, MNRAS, 440, 2333
Fioc, M., Rocca-Volmerange, B., 1997 and near submission
Fritz et al, 2006, MNRAS, 366, 767
Leitherer, C., 1999, ApJS, 123, 3
Noll etal., 2009, A&A, 507, 1793
Podigachoski, P., et al., 2015, A&A, 575, 80
Rocca-Volmerange, B., et al., 2013, MNRAS, 429, 78
Rocca-Volmerange, B., et al. 2015, ApJ, 808, L8
Siebenmorgen, 2015, arXiv 150804343
Wandelt , B., et al., arXiv 1211.2757