Paper: “Jet efficiencies and black hole spins in jetted quasars”

Black holes are fundamentally simple objects: only their mass and spin are enough to properly describe them. However, direct measurements of these two properties are not simple. Often, we look for observables which, upon being inserted in a physical model, may give us information about one of these fundamental properties of black holes. One such observable is luminosity. Our paper “Jet efficiencies and black hole spins in jetted quasars”, recently accepted by MNRAS (see preprint here), aims to relate jet properties with black hole spins.

With a sample of 154 flat-spectrum radio quasars (FSRQs), a subclass of blazars, whose masses had been previously estimated, we set out to find their gamma-ray luminosities in the Fermi 4FGL catalog, which comprises 8 years of observations performed with the Fermi Large Area Telescope (Fermi-LAT). Our first result is a correlation between jet luminosity and black hole mass, suggesting that more luminous jets are powered by more massive black holes.


We also estimated the jet power of these blazars. For this, we used a relation found in Nemmen et al. 2012. This, along with the assumption that these black holes are accreting at around 10 per cent of the Eddington rate — such high accretion rates are necessary for the thin discs believed to feed FSRQs — allowed us to estimate the jet efficiencies in these objects.


Having estimated the jet efficiencies, we used a simulation-based model to estimate the black hole spins. We found that, overall, these black holes are rotating very fast: the average spin was 0.84. This result is consistent with scenarios for the cosmological evolution of SMBHs which support rapidly rotating black holes as their host galaxies — and the black holes themselves — merge.

The preprint of the accepted version, with a full discussion, can be found here.

Chocolate, raclette and black holes

(with contributions by Ivan Almeida)

The Saas-Fee course is a yearly series of lectures usually held in the ski resort of Saas-Fee, Switzerland. This year, the 48th edition of the Saas-Fee course was held between 28th January and 3rd February, and was devoted to black holes. More specifically, the main subjects were black hole formation and growth. Four members of the group – Fábio, Gustavo, Ivan and Raniere – attended the event and presented their current work in the form of panels.

With about 130 participants coming from all over the world, the school was a valuable place to exchange experiences and ideas. The lectures, which were presented by professors Neil Cornish (Montana State University), Tiziana Di Mattteo (Carnegie Mellon University) and Andrew King (University of Leicester), focused on different aspects of black holes, including both theory and observations.

Professor Cornish covered theoretical and instrumental topics on mergers of compact objects as well as gravitational waves emerging from these events. He finished by including what we may expect in the next couple of years with the improvement of our current detectors’ capabilities and the addition of new gravitational wave detectors – both ground-based as well as the space-based LISA.

Professor Di Matteo’s lectures focused on the cosmological history of black holes, covering subjects like primordial black holes – and their possible origins -, first quasars and the current cosmological state of supermassive black holes in the center of galaxies.

Professor King presented a theoretical overview on accretion flows around black holes and black hole feedback, covering the formation and necessity for accretion flows, the black hole influence on its surroundings as well as a few open questions on the subject.

All lectures were very good, just like the chocolate and the cheese.

Saas-Fee is a little village in the Swiss Alps – a truly amazing view.

Multi-messenger astronomy: detection of gravitational waves and electromagnetic counterparts in neutron star merger

The most recent news in astronomy consists of the report that scientists have managed to record a collision of neutron stars in both gravitational waves and electromagnetic waves. This is a remarkable feat for many reasons. First of all, this is the first time that astronomers detected the gravitational waves that are produced when these neutron stars orbit each other in a deadly inspiral. Equally impressive was the fact that this event was also “seen”: it has been detected and monitored all across the electromagnetic spectrum. There were observations in gamma rays, X-rays, ultraviolet, visible light, infrared and radio. Moreover, the short gamma-ray burst detected shortly after the gravitational waves provided sound evidence that these bursts are associated with the collision of neutron stars. Finally, this merger has given us very sound evidence that such destructive events are responsible for the creation of heavy chemical elements in the periodic table, such as gold and platinum.

The gravitational waves, which are ripples in spacetime that occur when these massive objects orbit each other, were picked up by the LIGO twin detectors in the United States, as well as by Virgo, a gravitational wave detector in Italy. These are the same detectors that have been picking up gravitational waves from the mergers of black holes – the first detection gave 3 LIGO scientists the 2017 Nobel prize in Physics. However, this was the first time that scientists were able to detect gravitational waves from a merger of neutron stars, rather than black holes.

Just like black holes, neutron stars are one of the possible outcomes for a star when it runs out of fuel and collapses due to its own gravity. In order to become a neutron star, a star has to be very massive – much more than the Sun – but not extremely massive, otherwise it will collapse into a black hole. Mergers of black holes are thought to produce very little – if any – light, so they are difficult to “see” with traditional (electromagnetic) astronomy, although we are now able to “hear” them due to the gravitational waves produced in these collisions. Mergers of neutron stars, however, are a different story.

Less than two seconds after the gravitational waves were detected by LIGO and Virgo, the space telescope Fermi detected gamma rays coming from the same region where the gravitational waves came from. Alarms were sounded and telescopes all over the world, as well as in space, started to sweep the sky in order to pinpoint the location of this event. The Swope telescope, in Chile, was the first to report the location as the galaxy NGC 4993, in the constellation of Hydra, about 130 million light-years distant from the Earth.


Above, we see the detections of gravitational waves as well as observations across the entire electromagnetic spectrum. Source: LIGO.

The gamma rays detected by Fermi are what we call a short gamma-ray burst (sGRB). Before this detection, there were strong suggestions that these sGRB were produced when two neutron stars collide, but this was the first conclusive evidence that this is indeed what happens.

Once the telescopes were pointed to the sky, astronomers noticed a blob at the very place where this collision occurred. This blob is what we call a kilonova: a violent explosion that occurs when two neutron stars merge. Upon measuring the electromagnetic spectrum of this kilonova, astronomers detected the presence of heavy chemical elements, such as gold and platinum. This confirmed theoretical predictions that stated that these heavy elements are produced in such collisions, which are so strong that neutrons are literally forced into the nuclei of atoms, making them heavier and therefore creating heavier elements. This implies that the idea that we are all made of stardust also applies to our jewelry.

This detection of gravitational waves and the subsequent observation of this collision across all types of electromagnetic radiation marks the beginning of multi-messenger astronomy: we are now able to study the same event occurring in the universe using two very different types of information. It was a massive effort done by thousands of scientists scattered across the globe and is a small sample of the true power of scientific collaborations.