I started developing SÍGAME during my PhD at the Dark Cosmology Centre, a Center of Excellence in Denmark. Over the years, it grew into a mature software tool, rewritten in python and applicable to many cases of galaxy studies. I have led three first-author publications on SÍGAME and enjoyed working with team members from around the world, and the software tool is now available for download via GitHub.
Learn more about and download SÍGAME here›
At the Dark Cosmology Centre, I also worked on a more observational project which quantified the presence of active galactic nuclei (AGN) in massive galaxies at redshifts around 2 (about 10 billion years ago!) using CHANDRA archival X-ray data. High luminosity AGN are easily detected in X-ray at these redshifts, but to count the low luminosity AGN, it is necessary to apply some sort of stacking technique:
As an additional criteria when selecting AGN, the spectral shape of the X-ray emission can be used. For quantifying the slope of the X-ray spectra, astronomers typically use the observed “hardness ratio” between soft and hard X-ray flux. In the following figure from our paper, X-ray luminosity (on the y-axis) and hardness ratio (on the x-axis) are used to identify luminous AGN (filled symbols) and potential low-luminosity AGN (open symbols). Stacks of non-detections are shown with squares and blue and red colors signify star-forming and “quenched” galaxies, respectively:
We find in the paper that the low-luminosity AGN population constitutes a significant part of both the star-forming and the “quenched” galaxies at redshifts around 2. See my 2013 paper below for more details on the technique and results.
Keywords: Evolution of galaxies; Epoch of re-ionization; Interstellar Medium, Emission lines in radio; Radio interferometry; Galaxy simulations
My research focuses on the Interstellar Medium (ISM) of galaxies, i.e. that gas out of which stars are formed. The amount and properties of the ISM play a crucial role for the evolution of a galaxy, yet for galaxies at high redshifts both are poorly determined by observations. By observing a portion of ISM in different wavelengths, different images emerge, and astronomers can extract important information from each:
The best technique for observing the ISM is to look for emission lines in the infrared (left bottom panel above), where rotational lines of molecules and fine structure lines of atoms and ions are easily excited at typical ISM temperatures and densities.
2017: SÍGAME Simulations of the [CII], [OI], and [OIII] Line Emission from Star-forming Galaxies at z ~ 6 (ApJ 846 2, 2017)
2016: SImulator of GAlaxy Millimetre/submillimetre Emission (SÍGAME): CO emission from massive z = 2 main-sequence galaxies (MNRAS 457 3, 2016)
2015: Simulator of Galaxy Millimeter/Submillimeter Emission (SíGAME): The [CII]-SFR Relationship of Massive z = 2 Main Sequence Galaxies (ApJ 814 1, 2015)
2013: Measuring the AGN fraction among star-forming and quiescent galaxies at z~2 (ApJ 764 4, 2013)