Ciro Pinto

I am a senior staff scientist (Primo Ricercatore) at the Institute of Space Astrophysics and Cosmic Physics (INAF – IASF Palermo, Italy). My research focuses on the accretion of matter onto black holes at any mass scales and their feedback onto the surrounding interstellar medium of the host galaxy (primarily via winds) and galaxy cluster (via collimated jets).

I obtained my PhD at Radboud University Nijmegen in collaboration with SRON, the Netherlands Institute for Space Research with a thesis on the composition of the interstellar medium in the Galaxy as seen through X-rays. My master thesis at Naples University, Italy, focused on the X-ray variability of active galactic nuclei. More recently I have been 6 years in Cambridge, UK, working in the X-ray Group at the Institute of Astronomy, University of Cambridge. Before joining INAF I have been a Research Fellow for the European Space Agency at ESA / ESTEC in Noordwijk, Netherlands.

Ultra-luminous X-ray sources: relativistic winds

My team has observed two black holes in nearby galaxies devouring their companion stars at an extremely high rate, and spitting out matter at a quarter the speed of light (Image credit: ESA – C.Carreau). The two black holes NGC 1313 X-1 and NGC 5408 X-1, so bright in the X-ray energy band to be known as “ultra-luminous x-ray sources”, are sucking matter from their companion stars at a rate exceeding classically understood limits, and in the process, kicking out matter into surrounding space at astonishing speeds of around a quarter the speed of light. This discovery is crucial to understand the process of accretion onto compact objects and the physical phenomena that trigger the outflows of highly energetic winds. See also press release from the <European Space Agency (ESA)>, our original article published in <Nature> and a <TV interview>.

On the right there is a brand-new and more efficient contours visualisation of an outflowing plasma blowing at 17% of the speed of light in a supersoft ULX in the NGC 247 galaxy with very high significance achieved thanks to a deep observing campaign in the ESA’s XMM-Newton satellite (Pinto et al. 2021).

See e.g. my Webinar on ULXs and why Athena is the way to go

Exploding white dwarf Nova V2491 Cygni: 3000 km/s winds

A pioneer work. The X-ray spectrum at the outburst peak of this nova obtained with the RGS of XMM-Newton, shows deep absorption by ions of a wide range of ionization (e.g. O I-to-VIII). The deep absorption lines of the X-ray spectrum are divided in two main groups: the low-ionization absorption lines are at rest (v = 0 km/s) and are mostly due to the interstellar medium; the high-ionization absorption lines are blueshifted by about 3300 km/s and are produced in the ejecta. We model this expanding envelope with photo-ionized outflowing shells. The abundances of the shells indicate that they were ejected from an O-Ne white dwarf. Variations on time scales of hours in the X-ray spectrum are caused by a combination of variation in the central source and in the column density of the ionized shells. Our phenomenological model gives the best description so far of the supersoft X-ray spectrum of nova V2491 Cyg (Pinto et al. 2012b).

Hitomi first light of Perseus cluster of gakaxies: a surprisingly quiescent atmosphere

The Perseus galaxy cluster is filled with a hot X-ray-emitting gas, as seen in this image from NASA’s Chandra X-ray Observatory. Astronomers using the Soft X-ray Spectrometer aboard the Hitomi satellite have, for the first time, mapped the motion of this gas and determined its velocity structure across a large part of the cluster. The square overlay shows the area observed by Hitomi. The X-ray spectrum is also shown with emission from helium-like iron (that is iron with only 2 electrons) on the left and hydrogen-like iron (iron with only one electron) on the right. The narrowness of the emission lines shows that random motions in the 50 million K hot gas in the Perseus cluster core are only 164+/-10 km/s along the line-of-sight. This represents a dramatic improvement in the measurement precision of the velocities which are crucial for determining the total masses of clusters and the energy flow from the accreting black hole at the cluster centre. See also press release from the <European Space Agency (ESA)> and our original article published in <Nature>. (Copyright: Background: NASA/CXO; Spectrum: Hitomi Collaboration/JAXA, NASA, ESA, SRON, CSA).

Fornax A: an unusual “cooling” galaxy with a very powerful radio source

NGC 1316 (also known as Fornax A) is a lenticular galaxy about 60 million light-years away in the constellation Fornax. NGC 1316 is a radio galaxy. It is the fourth-brightest radio source in the sky (as seen at 1400 MHz). NGC 1316 is comparable to the giant elliptical galaxies found in the centers of other clusters of galaxies and hosts a hot gas with temperatures of several million degrees that strongly emits in the X-ray energy band. The image to the right shows the high-resolution XMM-Newton/RGS spectrum where I discovered -for the first time in an individual galaxy/cluster- the O VII lines which indicate gas cooling below 0.4 keV. This discovery is very useful to study the cooling of the intra-cluster/-group medium.

The interstellar matter can be modeled with a multi-phase gas plus dust grains. The gas has 3 main phases: neutral (O I), weakly ionized (O II-III) and highly ionized (O VII-VIII). Dust grains are still a quite open field. Both silicates and/or water amorphous ice are good candidates (Pinto et al. 2010-12a,c).