Associate researcher in the astronomy department of UCB, between 2000 and 2002,[1] he has since continued his scientific collaboration with researchers from several American institutes (UCB, UCLA,[2]University of Washington,[3]STScl.[4]) on various topics concerning globular clusters.
From 2007 to July 15, 2011, he was an astronomer in the instrumental division of the Baltimore Space Telescope Science Institute. He shares his work between scientific activities and functional tasks for the institute and for the Hubble Space Telescope Observatory (calibration, user support, maintenance missions and support of the institute in general).[9]
Luigi R. Bedin, principal investigator of major HST programs[11] is also leader of several observation projects for the world's main installations: HST, ESO/VLT,[12]LBT and the James Webb Space Telescope (JWST).[13][14]
He discovered, with his team, an isolated dwarf spheroidal galaxy as old as the universe hidden in NGC 6752. The discovery is published in international media in 2019. The galaxy bears his name: Bedin I.[17]
Bedin I Galaxy imaged by the Hubble Space Telescope
Research in astrometry and photometry from space with HST is enriched with JWST: calibration and instrumentation, extrasolar planets, clusters of globules.[21]
He is co-author of a study on intermediate black holes with the discovery of a homogeneous dark mass of around 800 M☉ corresponding to an intermediate mass black hole at the center of the cluster closest to Earth, the globular cluster Messier 4.[22]
In 2024, from JWST imaging of the nearest globular clusters, it detected excess infrared emission among white dwarfs in NGC 6397, a potential indication of destroyed ancient planetary systems and possible insights into the properties of the dense hydrogen atmosphere of these white dwarfs.[23]
NGC6397 region double observation HST and JWST
Tribute
2018: The dwarf galaxy Bedin I discovered with his team.[25]
↑ "Program Information". STScI.edu. Retrieved 2022-01-12. HST Programs With PI Last Name Similar To: bedin = 16653 - Luigi Bedin astrometric signature of a Second Planet in Proxima 15884 - Luigi Bedin Confirmation of an Astrometrically Detected Exoplanet Candidate Orbiting the closest Brown Dwarfs 15491 - Luigi Bedin The end of the White Dwarf Cooling Sequence of NGC 6752 15096 - Luigi Bedin The end of the White Dwarf Cooling Sequence of NGC 6752 14662 - Luigi Bedin The end of the White Dwarf Cooling Sequences of Omega Centauri 14330 - Luigi Bedin Astrometric search for Planets in the closest Brown Dwarf Binary system Luhman 16AB 14118 - Luigi Bedin The end of the White Dwarf Cooling Sequences of Omega Centauri 13748 - Luigi Bedin Astrometric search for Planets in the closest Brown Dwarf Binary system Luhman 16AB 12911 - Luigi Bedin A search for binaries with massive companions in the core of the closest globular cluster M4 12669 - Luigi Bedin Exploring the Bottom End of the White Dwarf Cooling Sequence in the Open Cluster NGC6819 11688 - Luigi Bedin Exploring the Bottom End of the White Dwarf Cooling Sequence in the Open Cluster NGC6819 10500 - Luigi Bedin Exploring the Bottom End of the White Dwarf Cooling Sequence in the Galactic Open Cluster NGC2158 10146 - Luigi Bedin Solving the problem of the White Dwarf Cooling Sequence End in M4: an efficent approach
↑ Galliani, Marco (2017-06-01). "Due nane brune per Hubble". MEDIA INAF (in Italian). Retrieved 2022-01-15. L'extraordinaire proximité de ce système en fait un laboratoire idéal pour étudier les propriétés des naines brunes, en particulier leurs atmosphères, l'évolution de leur température de surface, la nature binaire du système lui-même, et la présence éventuelle d'exoplanètes autour d'elles. Précisément sur ce dernier point Luigi Bedin, astronome de l'Institut national d'astrophysique (INAF) à l'Observatoire astronomique de Padoue, a récemment obtenu l'opportunité d'observer le système Luhman 16 avec le télescope spatial Hubble.
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A globular cluster is a spheroidal conglomeration of stars that is bound together by gravity, with a higher concentration of stars towards its center. It can contain anywhere from tens of thousands to many millions of member stars, all orbiting in a stable, compact formation. Globular clusters are similar in form to dwarf spheroidal galaxies, and the distinction between the two is not always clear. Their name is derived from Latin globulus. Globular clusters are occasionally known simply as "globulars".
An open cluster is a type of star cluster made of tens to a few thousand stars that were formed from the same giant molecular cloud and have roughly the same age. More than 1,100 open clusters have been discovered within the Milky Way galaxy, and many more are thought to exist. Each one is loosely bound by mutual gravitational attraction and becomes disrupted by close encounters with other clusters and clouds of gas as they orbit the Galactic Center. This can result in a loss of cluster members through internal close encounters and a dispersion into the main body of the galaxy. Open clusters generally survive for a few hundred million years, with the most massive ones surviving for a few billion years. In contrast, the more massive globular clusters of stars exert a stronger gravitational attraction on their members, and can survive for longer. Open clusters have been found only in spiral and irregular galaxies, in which active star formation is occurring.
Star clusters are large groups of stars held together by self-gravitation. Two main types of star clusters can be distinguished. Globular clusters are tight groups of ten thousand to millions of old stars which are gravitationally bound. Open clusters are more loosely clustered groups of stars, generally containing fewer than a few hundred members, that are often very young. As they move through the galaxy, over time, open clusters become disrupted by the gravitational influence of giant molecular clouds. Even though they are no longer gravitationally bound, they will continue to move in broadly the same direction through space and are then known as stellar associations, sometimes referred to as moving groups.
An elliptical galaxy is a type of galaxy with an approximately ellipsoidal shape and a smooth, nearly featureless image. They are one of the four main classes of galaxy described by Edwin Hubble in his Hubble sequence and 1936 work The Realm of the Nebulae, along with spiral and lenticular galaxies. Elliptical (E) galaxies are, together with lenticular galaxies (S0) with their large-scale disks, and ES galaxies with their intermediate scale disks, a subset of the "early-type" galaxy population.
The Eagle Nebula is a young open cluster of stars in the constellation Serpens, discovered by Jean-Philippe de Cheseaux in 1745–46. Both the "Eagle" and the "Star Queen" refer to visual impressions of the dark silhouette near the center of the nebula, an area made famous as the "Pillars of Creation" imaged by the Hubble Space Telescope. The nebula contains several active star-forming gas and dust regions, including the aforementioned Pillars of Creation. The Eagle Nebula lies in the Sagittarius Arm of the Milky Way.
Messier 4 or M4 is a globular cluster in the constellation of Scorpius. It was discovered by Philippe Loys de Chéseaux in 1745 and catalogued by Charles Messier in 1764. It was the first globular cluster in which individual stars were resolved.
NGC 6397 is a globular cluster in the constellation Ara that was discovered by French astronomer Nicolas-Louis de Lacaille in 1752. It is located about 7,800 light-years from Earth, making it one of the two nearest globular clusters to Earth. The cluster contains around 400,000 stars, and can be seen with the naked eye under good observing conditions.
Messier 2 or M2 is a globular cluster in the constellation Aquarius, five degrees north of the star Beta Aquarii. It was discovered by Jean-Dominique Maraldi in 1746, and is one of the largest known globular clusters.
Messier 12 or M 12 is a globular cluster in the constellation of Ophiuchus. It was discovered by the French astronomer Charles Messier on May 30, 1764, who described it as a "nebula without stars". In dark conditions this cluster can be faintly seen with a pair of binoculars. Resolving the stellar components requires a telescope with an aperture of 8 in (20 cm) or greater. In a 10 in (25 cm) scope, the granular core shows a diameter of 3′ (arcminutes) surrounded by a 10′ halo of stars.
NGC 6791 is an open star cluster in the Lyra constellation. It was discovered by Friedrich August Theodor Winnecke in 1853. At roughly 8 billion years old, and with an iron to hydrogen abundance ratio that is more than twice that of the Sun, it is one of the oldest and most metal-rich clusters in the Milky Way. This is contrary to the typical rule-of-thumb where older means more metal-poor. Compounded with the fact that it has an unusually high population of stars, NGC 6791 is among the most studied clusters in the sky.
NGC 3532, also commonly known as the Pincushion Cluster, Football Cluster, the Black Arrow Cluster, or the Wishing Well Cluster, is an open cluster some 405 parsecs from Earth in the constellation Carina. Its population of approximately 150 stars of 7th magnitude or fainter includes seven red giants and seven white dwarfs. On 20 May 1990 it became the first target ever observed by the Hubble Space Telescope. A line from Beta Crucis through Delta Crucis passes somewhat to the north of NGC 3532. The cluster lies between the constellation Crux and the larger but fainter "False Cross" asterism. The 4th-magnitude Cepheid variable star x Carinae appears near the southeast fringes, but it lies between the Sun and the cluster and is not a member of the cluster.
NGC 3201 is a low galactic latitude globular cluster in the southern constellation of Vela. It has a very low central concentration of stars. This cluster was discovered by James Dunlop on May 28, 1826 and listed in his 1827 catalogue. He described it as "a pretty large pretty bright round nebula, 4′ or 5′ diameter, very gradually condensed towards the centre, easily resolved into stars; the figure is rather irregular, and the stars are considerably scattered on the south".
NGC 6752 is a globular cluster in the constellation Pavo. It is the fourth-brightest globular cluster in the sky, after Omega Centauri, 47 Tucanae and Messier 22, respectively. It is best seen from June to October in the Southern Hemisphere.
Luhman 16 is a binary brown-dwarf system in the southern constellation Vela at a distance of 6.51 light-years from the Sun. These are the closest-known brown dwarfs and the closest system found since the measurement of the proper motion of Barnard's Star in 1916, and the third-closest-known system to the Sun. The primary is of spectral type L7.5 and the secondary of type T0.5 ± 1. The masses of Luhman 16 A and B are 35.4 and 29.4 Jupiter masses, respectively, and their ages are estimated to be 400–800 million years. Luhman 16 A and B orbit each other at a distance of about 3.5 astronomical units with an orbital period of approximately 26.6 years.
NGC 6388 is a globular cluster of stars located in the southern constellation of Scorpius. The cluster was discovered by Scottish astronomer James Dunlop on May 13, 1826 using a 20 cm (9 in) reflector telescope. It was later determined to be a globular cluster by English astronomer John Herschel, who was able to resolve it into individual stars. NGC 6388 is located at a distance of approximately 35,600 light-years (10.90 kpc) from the Sun. Due to its apparent visual magnitude of +6.8, binoculars or a small telescope are required to view it.
NGC 1755 is an open star cluster in the Large Magellanic Cloud in the Dorado constellation. It is about 120 light years across and due to its size could be a globular cluster. It has a diameter of 2.6′ and an apparent magnitude of 9.9. It was discovered by James Dunlop in 1826.
NGC 3311 is a super-giant elliptical galaxy located about 190 million light-years away in the constellation Hydra. The galaxy was discovered by astronomer John Herschel on March 30, 1835. NGC 3311 is the brightest member of the Hydra Cluster and forms a pair with NGC 3309 which along with NGC 3311, dominate the central region of the Hydra Cluster.
Bedin I is a dwarf spheroidal galaxy located in the constellation Pavo. It is situated around 28.38 million light-years from Earth, behind the globular cluster NGC 6752. Bedin I is possibly one of the oldest galaxies known, having formed around 10–13 billion years ago, and is one of the most isolated dwarf galaxies known, situated around 2.12 million light-years away from NGC 6744, its nearest neighbor with which it may be physically associated. As such, it has been deemed by astronomers as a "fossil" from the early universe. It was accidentally discovered by Italian astronomer Luigi Bedin, whose team was studying white dwarfs in NGC 6752 using the Hubble Space Telescope in September 2018; the discovery was announced in a paper published in January 2019.
Ata Sarajedini is an astrophysicist, professional astronomer, academic, author, and podcaster. He is the Bjorn Lamborn Endowed Chair and Professor in Astrophysics at Florida Atlantic University.
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