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Ginolfi M, Piconcelli E, Zappacosta L, Jones GC, Pentericci L, Maiolino R, Travascio A, Menci N, Carniani S, Rizzo F, Arrigoni Battaia F, Cantalupo S, De Breuck C, Graziani L, Knudsen K, Laursen P, Mainieri V, Schneider R, Stanley F, Valiante R, Verhamme A. Detection of companion galaxies around hot dust-obscured hyper-luminous galaxy W0410-0913. Nat Commun 2022; 13:4574. [PMID: 35931777 PMCID: PMC9355969 DOI: 10.1038/s41467-022-32297-x] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/12/2022] [Accepted: 07/22/2022] [Indexed: 11/28/2022] Open
Abstract
The phase transition between galaxies and quasars is often identified with the rare population of hyper-luminous, hot dust-obscured galaxies. Galaxy formation models predict these systems to grow via mergers, that can deliver large amounts of gas toward their centers, induce intense bursts of star formation and feed their supermassive black holes. Here we report the detection of 24 galaxies emitting Lyman-α emission on projected physical scales of about 400 kpc around the hyper-luminous hot dust-obscured galaxy W0410-0913, at redshift z = 3.631, using Very Large Telescope observations. While this indicates that W0410-0913 evolves in a very dense environment, we do not find clear signs of mergers that could sustain its growth. Data suggest that if mergers occurred, as models expect, these would involve less massive satellites, with only a moderate impact on the internal interstellar medium of W0410-0913, which is sustained by a rotationally-supported fast-rotating molecular disk, as Atacama Large Millimeter Array observations suggest. Lyman-alpha emission is one of the observational probes for the high-redshift universe. Here, the authors show several Lyman-alpha emitting companion galaxies around the hot dust-obscured galaxy W0410-091 suggesting that the galaxy evolves in a very dense environment.
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Affiliation(s)
- M Ginolfi
- European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748, Garching bei München, Germany.
| | - E Piconcelli
- INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040, Monte Porzio Catone, Italy
| | - L Zappacosta
- INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040, Monte Porzio Catone, Italy
| | - G C Jones
- Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford, OX1 4RH, UK.,Cavendish Laboratory, University of Cambridge, 19 J. J. Thomson Ave., Cambridge, CB3 0HE, UK.,Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK
| | - L Pentericci
- INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040, Monte Porzio Catone, Italy
| | - R Maiolino
- Cavendish Laboratory, University of Cambridge, 19 J. J. Thomson Ave., Cambridge, CB3 0HE, UK.,Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK
| | - A Travascio
- Department of Physics, University of Milan Bicocca, Piazza della Scienza 3, I-20126, Milano, Italy
| | - N Menci
- INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040, Monte Porzio Catone, Italy
| | - S Carniani
- Scuola Normale Superiore, Piazza dei Cavalieri 7, 56126, Pisa, Italy
| | - F Rizzo
- Cosmic Dawn Center (DAWN), Copenhagen, Denmark.,Niels Bohr Institute, University of Copenhagen, Jagtvej 128, DK-2200, Copenhagen N, Denmark
| | - F Arrigoni Battaia
- Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str 1, D-85748, Garching bei München, Germany
| | - S Cantalupo
- Department of Physics, University of Milan Bicocca, Piazza della Scienza 3, I-20126, Milano, Italy
| | - C De Breuck
- European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748, Garching bei München, Germany
| | - L Graziani
- Dipartimento di Fisica, Sapienza, Universita di Roma, Piazzale Aldo Moro 5, I-00185, Roma, Italy
| | - K Knudsen
- Department of Space, Earth, and Environment, Chalmers University of Technology, Onsala Space Observatory, SE-439 92, Onsala, Sweden
| | - P Laursen
- Cosmic Dawn Center (DAWN), Copenhagen, Denmark.,Niels Bohr Institute, University of Copenhagen, Jagtvej 128, DK-2200, Copenhagen N, Denmark
| | - V Mainieri
- European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748, Garching bei München, Germany
| | - R Schneider
- Dipartimento di Fisica, Sapienza, Universita di Roma, Piazzale Aldo Moro 5, I-00185, Roma, Italy
| | - F Stanley
- Sorbonne Université, UPMC Université Paris 6 & CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98b boulevard Arago, 75014, Paris, France
| | - R Valiante
- INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040, Monte Porzio Catone, Italy
| | - A Verhamme
- Observatoire de Genéve, Université de Genève, 51 Ch. des Maillettes, 1290, Versoix, Switzerland
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Abstract
The flattening of spiral-galaxy rotation curves is unnatural in view of the expectations from Kepler’s third law and a central mass. It is interesting, however, that the radius-independence velocity is what one expects in one less dimension. In our three-dimensional space, the rotation curve is natural if, outside the galaxy’s center, the gravitational potential corresponds to that of a very prolate ellipsoid, filament, string, or otherwise cylindrical structure perpendicular to the galactic plane. While there is observational evidence (and numerical simulations) for filamentary structure at large scales, this has not been discussed at scales commensurable with galactic sizes. If, nevertheless, the hypothesis is tentatively adopted, the scaling exponent of the baryonic Tully–Fisher relation due to accretion of visible matter by the halo comes out to reasonably be 4. At a minimum, this analytical limit would suggest that simulations yielding prolate haloes would provide a better overall fit to small-scale galaxy data.
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