Galaxy group and cluster.

Supermassive black holes and AGN.

Galaxy formation and evolution.

Projects and Research

The Galaxy

A galaxy is a dynamically bound system that consists of billions of stars, gas and dust, and dark matter. They can be found in isolation but the majority of them are found in galaxy groups and clusters. The morphology and star formation activities of galaxies in clusters differ from those in isolation which points at the morphology-density relations. Based on what we know today, there is much more into the role of environments in galaxy formation than what can be deduced based on a simple classification of environment e.g. field, groups and clusters.


The Radio Semi-Analytic Galaxy Evolution model, or Radio-SAGE as fork of the main SAGE model that is a publicly available codebase for exploring galaxy formation in a cosmological context with prediction of relativistic jet properties of luminous galaixies. The main SAGE model, described in Croton et al. (2016) and Radio-SAGE describe by Raouf et al. in which submitted for publication in MNRAS. SAGE will run on any N-body simulation whose trees are organised in a supported format and contain a minimum set of basic halo properties.

Group & Cluster

A significant fraction of galaxies are settled into groups and clusters in which the number density of galaxies is around tens to a few hundred times higher than the average number density in the Universe. There are considerable diversities between galaxy populations in the field and those in clusters (The densest and most populous of galaxies aggregations are called galaxy clusters, which typically contain more than 50 relatively bright galaxies in a volume only a few Mpc across) and groups (The smaller, less populous aggregations of galaxies).

Black Holes, Quasars, and Radio AGN

Black holes are now thought to play a central role in shaping the evolution of galaxies. As quasars, the can shine brighter than all the stars in the galaxy, triggered from the violence of a galaxy-galaxy collision. Late in its life the black hole shifts to a low accretion state that can inject just enough energy into the surrounding galaxy so-as to starve the galaxy of any future star forming material. These (relatively) tiny objects have the potential to dramatically alter galactic evolution, making them critical objects of study.

The Environmental Dependence of Galaxy Formation

With the flood of quality data provided by galaxy surveys we have only recently been able to study galaxies across the full spectrum of environments. Naively, one would expect environment to be of great importance in shaping galactic growth. Interestingly however, environment appears to play second fiddle to a much a more fundamental factor: the mass of the galaxy's dark matter halo. Understanding exactly why this is and what processes are at play is of great importance.

Virialized galaxy systems

The dominant force on large scales structure of the Universe is gravity, which shapes the development of structure through the collapse and subsequent formation of virialized objects, where equilibrium is maintained by the balance between the gravitational energy associated with the mass of the system and the kinetic energy of its individual components. The largest such organized structures are clusters of galaxies, in which many hundreds or thousands of individual galaxies are gravitationally bound by the presence of a large mass concentration arranged in an extended halo. By definition a system is relaxed when no information remains about the initial orbits of most of its particles.


My full list of publications are accessible through the SAO/NASA Astrophysics Data System,
sorted chronologically here, and by “popularity” here.

Radio-SAGE data

The catalogues of Radio-SAGE groups, group properties and galaxy properties are publicly available on coming soon.

Lecture video : Galaxy Formation - Farsi

Astrophysics lecture - Galaxy formation by Mojtaba Raouf. (pdf file)

About Me

I am an observational and numerical astrophysicist, focusing on the formation and evolution of galaxies in the local Universe, using both simulations and large observational data sets.

I work as a Postdoctoral of Astrophysics in the School of Astronomy at Institute for research in fundamental science in Tehran, Iran.


Have a question? Contact me!

School of Astronomy
Institute for research in fundamental science- IPM
Mail Number Tehran, 19395-5531, Iran

Visit the Centre! Directions can be found here.
Office: SoA10
Phone: +98-21-23105067
Fax +98-21-23105067

Or contact me via Email email or Telegram Telegram