Molecular hydrogen (H2) makes up 99% of the cold dense gas in galaxies. So mapping where stars are born basically means measuring H2, which lacks a strong characteristic signature at low temperatures. Astronomers from SRON Netherlands Institute for Space Research and the University of Groningen have now mapped an emission signal from the trace molecule hydrogen fluoride (HF), in a place where the standard trace molecule carbon monoxide is absent. They are the first to produce a map of HF for a region in space, creating a new tool to indirectly map H2. Publication in Astronomy & Astrophysics on November 6th.
All across galaxies in our Universe, stars are dying and forming. And while our life on Earth is based on a rich jumble of various elements and molecules, the cold dense gas out of which stars form is pretty monotonous with 99% molecular hydrogen (H2). So if you want to map where stars are born, you’d better have a good grasp on how to detect H2. Unfortunately, this material is hard to observe due to a lack of a strong characteristic signal at low temperatures—unlike its atomic cousin (H) which emits radio waves at an easily distinguishable wavelength of 21 cm. Astronomers from SRON Netherlands Institute for Space Research and the University of Groningen have now discovered a new tool to indirectly measure H2, by mapping hydrogen fluoride (HF) and linking its abundance to that of H2.
The new tool comes in handy when other tools fail, for example in the Orion Bar, in between regions around the Orion Trapezium stars, and the Orion Molecular Cloud. In these areas carbon is ionized, meaning that carbon monoxide (CO)—usually a reliable trace molecule to find H2—can’t work as a tracer in this case. Floris van der Tak (SRON/RuG) and his team were surprised to find a characteristic HF signal in data from the Herschel telescope coming from the Orion Bar, as astronomers have previously only detected hydrogen fluoride as a silhouette: HF absorbing other radiation. HF and H2 abundance can be linked because HF is produced in a chemical reaction where H2 reacts with atomic fluorine (F) to form HF and atomic hydrogen (H). Without H2 there is no HF.
The team, led by SRON Ph.D. student Ümit Kavak, used their map of HF to examine a few mechanisms through which it could emit its signal. Collisions of HF molecules with electrons and molecular hydrogen turn out to be the main mechanism. The collisions excite the HF molecules to a higher energy state, after which they drop to their ground state while emitting infrared light at a characteristic wavelength of 1.2 THz.
“Origin of hydrogen fluoride emission in the Orion Bar: An excellent tracer for CO-dark H2 gas clouds” by Ü. Kavak, F. F. S. van der Tak, A. G. G. M. Tielens and R. F. Shipman, 6 November 2019, Astronomy & Astrophysics.
Chandaryaan2 3D images https://www.sarthtya.tech/2019/11/chandaryaan2-chandaryaan2-send-their.html?m=1