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arxiv: 2606.25051 · v1 · pith:DQDQDABDnew · submitted 2026-06-23 · 🌌 astro-ph.GA

The Nearest Galactic Nucleus: Studying the Galactic Centre with SKA-Mid

Rainer Schoedel , Antxon Alberdi , Izaskun Jim\'enez-Serra , Michael Kramer , Farhad Yusef-Zadeh , Miguel P\'erez-Torres , Mark R. Morris , Rob Fender
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Jan Forbrich Adriano Ingallinera Miguel Cano-Gonz\'alez Jonathan D. Henshaw Steven Longmore Javier Mold\'on Angela Gardini Ian Heywood Isabella Rammala Fatemeh Tabatabaei Farideh Mazoochi Veena Vadamattom Alessio Traficante Michal Zajacek Jaroslav Haas Lourdes Verdes-Montenegro Susana S\'anchez-Exp\'osito Alvaro Mart\'inez-Arranz Francisco Nogueras-Lara
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Pith reviewed 2026-06-25 23:22 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords Galactic CentreSKA-MidSagittarius A*nuclear star clustercontinuum surveygalactic nucleistellar remnantsstar formation rate
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The pith

A single SKA-Mid survey of the Galactic Centre can tackle multiple nuclear physics questions with one dataset.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper positions the Galactic Centre as the nearest galactic nucleus and the most extreme observable environment in the Milky Way, unmatched in stellar density, interstellar medium conditions, magnetic fields, and star formation rate. It argues that a 2.0 by 0.4 degree multi-wavelength continuum survey centered on Sagittarius A* plus repeated deep observations of the nuclear star cluster over a decade would let researchers study rare objects such as extremely massive stars and stellar remnants at a known distance. The approach is presented as efficient because one dataset can serve many distinct science problems instead of requiring separate targeted campaigns. The proposal rests on the idea that the well-defined distance to the Galactic Centre turns it into a calibrated laboratory for understanding galactic nuclei in general.

Core claim

The Galactic Centre is the nearest nucleus of a galaxy and the most extreme environment observable down to physical scales of a few hundred astronomical units, with no other Milky Way region matching its stellar density, turbulence, temperature, large-scale magnetic field, concentration of stellar remnants, or mean star formation rate. A large-area multi-wavelength continuum survey with SKA-Mid covering about 2.0 deg by 0.4 deg centred on Sagittarius A* together with repeated deep observations of the nuclear star cluster over a decade will allow the community to address multiple science problems with a single dataset.

What carries the argument

The proposed SKA-Mid large-area multi-wavelength continuum survey of 2.0 by 0.4 degrees plus decade-long repeated deep observations of the nuclear star cluster.

If this is right

  • Detection and study of extremely massive stars and stellar remnants becomes possible at a single well-known distance.
  • The physics of galactic nuclei can be examined in detail through the unique conditions of stellar density and magnetic fields.
  • Properties of the interstellar medium such as turbulence, temperature, and large-scale magnetic field strength can be mapped comprehensively.
  • The mean star formation rate in an extreme environment can be measured directly.
  • Time-domain phenomena can be tracked through repeated observations spanning a decade.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The resulting catalog could act as a local benchmark for interpreting observations of more distant galactic nuclei with future instruments.
  • The wide-field data might uncover unexpected populations of objects or structures not highlighted in the listed science cases.
  • Comprehensive census information could tighten constraints on models of how the central black hole interacts with its surrounding stellar and gaseous environment.

Load-bearing premise

That the planned SKA-Mid sensitivity, angular resolution, and survey parameters will be delivered as expected and will prove sufficient to address the listed science problems without needing substantial extra targeted observations.

What would settle it

A test observation or simulation showing that the angular resolution or sensitivity at the required frequencies falls short of what is needed to resolve or detect the targeted stellar remnants and massive stars at distances of a few hundred AU from Sagittarius A*.

Figures

Figures reproduced from arXiv: 2606.25051 by Adriano Ingallinera, Alessio Traficante, Alvaro Mart\'inez-Arranz, Angela Gardini, Antxon Alberdi, Farhad Yusef-Zadeh, Farideh Mazoochi, Fatemeh Tabatabaei, Francisco Nogueras-Lara, Ian Heywood, Isabella Rammala, Izaskun Jim\'enez-Serra, Jan Forbrich, Jaroslav Haas, Javier Mold\'on, Jonathan D. Henshaw, Lourdes Verdes-Montenegro, Mark R. Morris, Michael Kramer, Michal Zajacek, Miguel Cano-Gonz\'alez, Miguel P\'erez-Torres, Rainer Schoedel, Rob Fender, Steven Longmore, Susana S\'anchez-Exp\'osito, Veena Vadamattom.

Figure 1
Figure 1. Figure 1: Left: Schematic view of our Galaxy (thanks to M. Sormani for the sketch). The red circle outlines the location and size of the CMZ and NSD. Right: Spitzer 3.6 + 4.5 + 8.0 𝜇m image of the GC. The NSC surrounds Sgr A* and lies embedded in the NSD. The majority of the molecular gas in the CMZ is concentrated within the blue, dotted ellipse, which contains several prominent infrared dark clouds. In addition to… view at source ↗
Figure 2
Figure 2. Figure 2: Radio-X-ray correlation for NS and BH LMXBs in the hard state located at the distance of the GC. The blue line/shaded region shows the radio-X-ray correlation for BH LMXBs and the green line/shaded region shows the one for NS LMXBs according to Gallo et al. (2018). Distinguishing between NS and BH LMXBs is of critical importance when studying their numbers, distribution, and properties. With their relative… view at source ↗
Figure 3
Figure 3. Figure 3: Cumulative radio luminosity functions (RLFs) for a star-forming event of 2×104 M⊙ at the distance of the GC with different assumed ages and solar metallicity. The prediction are based on MIST isochrones, using SPISEA to simulate clusters, assuming an initial mass function with slope −1.8 (Hosek et al., 2019). The mass-loss rates of the stars that are provided by the MIST models were converted to radio lumi… view at source ↗
Figure 4
Figure 4. Figure 4: Flux densities of different types of radio point sources that we can expect to detect at the GC (solid lines). Vertical dotted lines indicate the central frequencies of bands 2 (1.355 GHz), 5a (6.55 GHz), and 5b (11.85 GHz). The dashed gray to black lines indicate the 3 𝜎 rms of SKA1-Mid for integration times of 1 h, 10 h, and 100 h. The dash-dotted brown line indicates the 3 𝜎 rms of the current JVLA. A G… view at source ↗
Figure 5
Figure 5. Figure 5: Possible layout of pointings at 12.5 GHz, overlaid over a Spitzer 3.6 𝜇m image. Galactic north is up, Galactic east is to the left. The NSC is shown in the zoomed inlet, with the 11.85 GHZ primary beam overplotted. The four disconnected circles to the Galactic north are comparison fields in the inner Galactic bar. This shallow survey should be complemented by repeated deep observations of the NSC. We propo… view at source ↗
read the original abstract

The Galactic Centre is the nearest nucleus of a galaxy and the most extreme environment that we can observe down to physical scales of a few hundred astronomical units. There is no other region in the Milky Way that can match its unique characteristics, such as its stellar density, turbulence and temperature of the interstellar medium, strong large scale magnetic field, concentration of stellar remnants, or mean star formation rate. The Galactic Centre is a unique target to understand the physics of galactic nuclei and study a large number of rare objects, such as extremely massive stars and stellar remnants, at a well-defined distance. The Galactic Centre has been and is being studied intensively with the most advanced facilities. In this chapter, we advocate for a large-area, multi-wavelength continuum survey with the Square Kilometre Array of an area of about 2.0deg x 0.4deg (~290pc x 60pc), centred on the massive black hole Sagittarius A* and for repeated deep observations of the nuclear star cluster over a decade, which will allow the community to address multiple science problems with single dataset.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 0 minor

Summary. The manuscript presents a science case advocating a large-area (approximately 2.0° × 0.4°, or ~290 pc × 60 pc), multi-wavelength continuum survey with SKA-Mid centered on Sagittarius A* in the Galactic Centre, together with repeated deep observations of the nuclear star cluster spanning a decade. It argues that this single dataset would enable the community to address multiple science problems, including the physics of galactic nuclei, the study of rare objects such as extremely massive stars and stellar remnants, and properties of the interstellar medium in this extreme environment.

Significance. If the proposed survey parameters prove feasible, the resulting high-resolution, multi-epoch radio data on the nearest galactic nucleus would provide a valuable resource for studying stellar populations, magnetic fields, and black-hole environments at scales of a few hundred AU, with potential to inform models of galactic nuclei across the Universe.

major comments (1)
  1. [Abstract] Abstract: the central claim that the proposed survey 'will allow the community to address multiple science problems with single dataset' lacks any supporting quantitative sensitivity calculations, simulations, or error analysis showing that the stated area, depth, cadence, and multi-wavelength coverage are sufficient to deliver the listed science goals without additional targeted observations.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive feedback on our science case for an SKA-Mid survey of the Galactic Centre. We address the single major comment below.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central claim that the proposed survey 'will allow the community to address multiple science problems with single dataset' lacks any supporting quantitative sensitivity calculations, simulations, or error analysis showing that the stated area, depth, cadence, and multi-wavelength coverage are sufficient to deliver the listed science goals without additional targeted observations.

    Authors: We agree that the abstract presents a strong claim without accompanying quantitative support. The manuscript is structured as a high-level science case chapter rather than a detailed technical proposal, with the body providing qualitative justification drawn from existing multi-wavelength data on the Galactic Centre. To address this point directly, we will revise the abstract and add a concise new subsection (or expanded paragraph in the introduction) that includes order-of-magnitude sensitivity estimates using published SKA-Mid performance specifications for the primary goals, such as detection thresholds for stellar remnants, magnetic field mapping via synchrotron emission, and variability monitoring of Sgr A*. Full end-to-end simulations and formal error budgets lie outside the scope of this advocacy paper and would require dedicated follow-up work; we will note this limitation explicitly in the revision. revision: partial

Circularity Check

0 steps flagged

No significant circularity in this science proposal

full rationale

This manuscript is a science-case proposal advocating SKA-Mid observations of the Galactic Centre. It contains no mathematical derivations, model fits, quantitative predictions, or equations whose outputs could reduce to their inputs. The recommendation rests on established external knowledge of the target region rather than any self-referential logic, self-citation chains, or fitted parameters renamed as predictions. No circular steps are present.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

This is an observational advocacy paper with no mathematical model, free parameters, axioms, or new entities introduced.

pith-pipeline@v0.9.1-grok · 5867 in / 1119 out tokens · 30716 ms · 2026-06-25T23:22:17.266053+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

107 extracted references · 107 canonical work pages · 2 internal anchors

  1. [1]

    doi: 10.1088/0004-637X/697/2/

    work page doi:10.1088/0004-637x/697/2/

  2. [2]

    doi: 10.3847/1538-4357/abadf6. A. Báez-Rubio et al.A&A, 571:L4, Nov

    work page doi:10.3847/1538-4357/abadf6

  3. [3]

    doi: 10.1051/0004-6361/201424389. J. Bally et al.arXiv e-prints, art. arXiv:2412.10983, Dec

    work page doi:10.1051/0004-6361/201424389

  4. [4]

    doi: 10.48550/arXiv.2412.10983. H. Bartko et al.ApJ, 708:834–840, Jan

    work page doi:10.48550/arxiv.2412.10983

  5. [5]

    doi: 10.1088/0004-637X/708/1/834. H. Baumgardt, P. Amaro-Seoane, and R. Schödel.A&A, 609:A28, Jan

    work page doi:10.1088/0004-637x/708/1/834

  6. [6]

    doi: 10.1111/j.1365-2966.2006.10467.x. H. K. Bhat et al.ApJ, 929(2):178, Apr

    work page doi:10.1111/j.1365-2966.2006.10467.x 2006

  7. [7]

    doi: 10.3847/1538-4357/ac6106. E. Bianchi et al.ApJ, 944(2):208, Feb

    work page doi:10.3847/1538-4357/ac6106

  8. [8]

    doi: 10.3847/1538-4357/acb5e8. L. A. Busch et al.A&A, 668:A183, Dec

    work page doi:10.3847/1538-4357/acb5e8

  9. [9]

    doi: 10.1051/0004-6361/202244870. M. Cano-González et al.A&A, 692:A23, Dec

    work page doi:10.1051/0004-6361/202244870

  10. [10]

    doi: 10.1051/0004-6361/202451771. M. Cano-González et al.A&A, 700:A246, Aug

    work page doi:10.1051/0004-6361/202451771

  11. [11]

    doi: 10.1051/0004-6361/202554533. J. S. Clark et al.A&A, 649:A43, May

    work page doi:10.1051/0004-6361/202554533

  12. [12]

    doi: 10.1051/0004-6361/202039205. J. S. Clark et al.MNRAS, 521(3):4473–4489, May

    work page doi:10.1051/0004-6361/202039205

  13. [13]

    doi: 10.1093/mnras/stad449. S. Corbel et al.MNRAS, 428(3):2500–2515, Jan

    work page doi:10.1093/mnras/stad449

  14. [14]

    doi: 10.1093/mnras/sts215. P. de Vicente, J. Martín-Pintado, R. Neri, and P. Colom.A&A, 361:1058–1072, Sept

    work page doi:10.1093/mnras/sts215

  15. [15]

    doi: 10.48550/arXiv.astro-ph/0009195. J. S. Deneva, J. M. Cordes, and T. J. W. Lazio.ApJ, 702(2):L177–L181, Sept

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0009195

  16. [16]

    doi: 10.1088/0004-637X/702/2/L177. J. Dexter and R. M. O’Leary.ApJ, 783(1):L7, Mar

    work page doi:10.1088/0004-637x/702/2/l177

  17. [17]

    doi: 10.1088/2041-8205/783/1/L7. H. Dong et al.MNRAS, 417:114–135, Oct

    work page doi:10.1088/2041-8205/783/1/l7 2041

  18. [18]

    2011, MNRAS, 417, 2571, doi: 10.1111/j.1365-2966.2011.19423.x

    doi: 10.1111/j.1365-2966.2011.19013.x. 21 The Galactic Centre Schödel et al. R.Eatoughetal. InAdvancingAstrophysicswiththeSquareKilometreArray(AASKA14),page45, Apr

    work page doi:10.1111/j.1365-2966.2011.19013.x 2011

  19. [19]

    doi: 10.1086/175498. A. Feldmeier-Krause et al.MNRAS, 466:4040, May

    work page doi:10.1086/175498

  20. [20]

    doi: 10.1093/mnras/stw3377. R. P. Fender, T. M. Belloni, and E. Gallo.MNRAS, 355(4):1105–1118, Dec

    work page doi:10.1093/mnras/stw3377

  21. [21]

    1937-5956.2010.01194.x

    doi: 10.1111/j. 1365-2966.2004.08384.x. G. Fragione, B. Kocsis, F. A. Rasio, and J. Silk.ApJ, 927(2):231, Mar

    work page doi:10.1111/j 2004

  22. [22]

    M.Freitag,P.Amaro-Seoane,andV.Kalogera.ApJ,649:91–117,Sept.2006

    doi: 10.3847/ 1538-4357/ac5026. M.Freitag,P.Amaro-Seoane,andV.Kalogera.ApJ,649:91–117,Sept.2006. doi: 10.1086/506193. A. T. Gallego-Calvente et al.A&A, 647:A110, Mar

    work page doi:10.1086/506193 2006

  23. [23]

    doi: 10.1051/0004-6361/202039172. A. T. Gallego-Calvente et al.A&A, 664:A49, Aug

    work page doi:10.1051/0004-6361/202039172

  24. [24]

    doi: 10.1051/0004-6361/202141895. E. Gallego-Cano et al.A&A, 634:A71, Feb

    work page doi:10.1051/0004-6361/202141895

  25. [25]

    doi: 10.1051/0004-6361/201935303. E. Gallo et al.MNRAS, 445(1):290–300, Nov

    work page doi:10.1051/0004-6361/201935303

  26. [26]

    doi: 10.1093/mnras/stu1599. E. Gallo, N. Degenaar, and J. van den Eijnden.MNRAS, 478(1):L132–L136, Jul

    work page doi:10.1093/mnras/stu1599

  27. [27]

    doi: 10.1093/mnrasl/sly083. G. Garay and S. Lizano.PASP, 111(763):1049–1087, Sept

    work page doi:10.1093/mnrasl/sly083

  28. [28]

    doi: 10.1086/316416. A. Generozov, N. C. Stone, B. D. Metzger, and J. P. Ostriker.MNRAS, May

    work page doi:10.1086/316416

  29. [29]

    R.Genzel, F.Eisenhauer, andS.Gillessen.ReviewsofModernPhysics, 82:3121–3195, Oct.2010

    doi: 10.1093/ mnras/sty1262. R.Genzel, F.Eisenhauer, andS.Gillessen.ReviewsofModernPhysics, 82:3121–3195, Oct.2010. doi: 10.1103/RevModPhys.82.3121. Gravity Collaboration et al.A&A, 636:L5, Apr

    work page doi:10.1103/revmodphys.82.3121 2010

  30. [30]

    doi: 10.1051/0004-6361/202037813. J. E. Greene, J. Strader, and L. C. Ho.ARA&A, 58:257–312, Aug

    work page doi:10.1051/0004-6361/202037813

  31. [31]

    doi: 10.1051/0004-6361/ 202453324. C. J. Hailey et al.Nature, 556:70–73, Apr

    work page doi:10.1051/0004-6361/

  32. [32]

    doi: 10.1038/nature25029. N. Harada et al.ApJ, 884(2):100, Oct

    work page doi:10.1038/nature25029

  33. [33]

    doi: 10.3847/1538-4357/ab41ff. H. Hassani et al.MNRAS, 510(1):11–31, Feb

    work page doi:10.3847/1538-4357/ab41ff

  34. [34]

    doi: 10.1093/mnras/stab3202. J. D. Henshaw et al. In S. Inutsuka et al., editors,Protostars and Planets VII, volume 534 of Astronomical Society of the Pacific Conference Series, page 83, July

    work page doi:10.1093/mnras/stab3202

  35. [35]

    In: Proceedings of the 5th Con- ference on Robot Learning, pp

    doi: 10.48550/arXiv. 2203.11223. I. Heywood et al.Nature, 573(7773):235–237, Sept. 2019a. doi: 10.1038/s41586-019-1532-5. I. Heywood et al.Nature, 573(7773):235–237, Sep 2019b. doi: 10.1038/s41586-019-1532-5. I. Heywood et al.arXiv e-prints, art. arXiv:2201.10541, Jan

    work page internal anchor Pith review doi:10.48550/arxiv

  36. [36]

    Modeling and simulation of wear in revolute clearance joints in multi- body systems.Mechanism and Machine Theory, 44(6):1211–1222, 2009

    doi: 10.1016/j. physletb.2011.02.029. J. Hosek, Matthew W. et al.ApJ, 870(1):44, Jan

    work page doi:10.1016/j 2011

  37. [37]

    doi: 10.3847/1538-4357/aaef90. J. Hosek, Matthew W. et al.AJ, 160(3):143, Sept

    work page doi:10.3847/1538-4357/aaef90

  38. [38]

    doi: 10.3847/1538-3881/aba533. S. E. Hosseini et al.ApJ, 975(2):261, Nov

    work page doi:10.3847/1538-3881/aba533

  39. [39]

    doi: 10.3847/1538-4357/ad7d06. B. Hußmann et al.A&A, 540:A57, Apr

    work page doi:10.3847/1538-4357/ad7d06

  40. [40]

    doi: 10.1051/0004-6361/201117637. F. Jankowski et al.MNRAS, 473(4):4436–4458, Feb

    work page doi:10.1051/0004-6361/201117637

  41. [41]

    doi: 10.1093/mnras/stx2476. I. Jiménez-Serra et al.Astrobiology, 20(9):1048–1066, Sept

    work page doi:10.1093/mnras/stx2476

  42. [42]

    doi: 10.1089/ast.2019.2125. I. Jiménez-Serra et al.Frontiers in Astronomy and Space Sciences, 9:843766, Mar. 2022a. doi: 22 The Galactic Centre Schödel et al. 10.3389/fspas.2022.843766. I. Jiménez-Serra et al.A&A, 663:A181, July 2022b. doi: 10.1051/0004-6361/202142699. A. Karska et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1089/ast.2019.2125 2019

  43. [43]

    doi: 10.1142/S0218271816300299. M. Kramer et al.New A Rev., 48(11-12):993–1002, Dec

    work page doi:10.1142/s0218271816300299

  44. [44]

    doi: 10.1016/j.newar.2004.09.020. J. M. D. Kruijssen and S. N. Longmore.MNRAS, 435(3):2598–2603, Nov

    work page doi:10.1016/j.newar.2004.09.020 2004

  45. [45]

    doi: 10.1093/mnras/stu494. M. Labaj et al.A&A, 702:A233, Oct

    work page doi:10.1093/mnras/stu494

  46. [46]

    doi: 10.1051/0004-6361/202554982. C. C. Lang, K. E. Johnson, W. M. Goss, and L. F. Rodríguez.AJ, 130:2185–2196, Nov

    work page doi:10.1051/0004-6361/202554982

  47. [47]

    doi: 10.1086/496976. M. A. Latif, D. R. G. Schleicher, W. Schmidt, and J. C. Niemeyer.MNRAS, 436(4):2989–2996, Dec

    work page doi:10.1086/496976

  48. [48]

    R.Launhardt,R.Zylka,andP.G.Mezger.A&A,384:112–139,Mar.2002.doi: 10.1051/0004-6361: 20020017

    doi: 10.1093/mnras/stt1786. R.Launhardt,R.Zylka,andP.G.Mezger.A&A,384:112–139,Mar.2002.doi: 10.1051/0004-6361: 20020017. C. Leitherer, J. M. Chapman, and B. Koribalski.ApJ, 481(2):898–911, May

    work page doi:10.1093/mnras/stt1786 2002

  49. [49]

    doi: 10.1088/0004-637X/747/1/1. A. Loeb and F. A. Rasio.ApJ, 432:52, Sept

    work page doi:10.1088/0004-637x/747/1/1

  50. [50]

    doi: 10.1086/174548. S. N. Longmore et al.MNRAS, 429(2):987–1000, Feb

    work page doi:10.1086/174548

  51. [51]

    doi: 10.1093/mnras/sts376. M. E. Lower, S. Dai, and S. Johnston.arXiv e-prints, art. arXiv:2404.09098, Apr

    work page doi:10.1093/mnras/sts376

  52. [52]

    doi: 10.48550/arXiv.2404.09098. J. R. Lu et al.ApJ, 764:155, Feb

    work page doi:10.48550/arxiv.2404.09098

  53. [53]

    doi: 10.1088/0004-637X/764/2/155. P. Madau and M. J. Rees.ApJ, 551(1):L27–L30, Apr

    work page doi:10.1088/0004-637x/764/2/155

  54. [54]

    doi: 10.1086/319848. S. Mandel et al.ApJ, 985(2):202, June

    work page doi:10.1086/319848

  55. [55]

    doi: 10.3847/1538-4357/adc07e. S. Martín et al.A&A, 656:A46, Dec

    work page doi:10.3847/1538-4357/adc07e

  56. [56]

    doi: 10.1051/0004-6361/202141567. J. Martín-Pintado et al.ApJ, 628(1):L61–L64, July

    work page doi:10.1051/0004-6361/202141567

  57. [57]

    doi: 10.1086/432684. Á. Martínez-Arranz et al.A&A, 683:A3, Mar. 2024a. doi: 10.1051/0004-6361/202347937. A. Martínez-Arranz et al.A&A, 685:L7, May 2024b. doi: 10.1051/0004-6361/202449877. Á. Martínez Arranz, R. Schödel, H. Bouy, and F. Nogueras-Lara.arXiv e-prints, art. arXiv:2510.11966, Oct

    work page doi:10.1086/432684

  58. [58]

    doi: 10.3847/1538-4357/acebcd. J. C. Mauerhan et al.ApJ, 710:706–728, Feb

    work page doi:10.3847/1538-4357/acebcd

  59. [59]

    doi: 10.1088/0004-637X/710/1/706. F. Mazoochi et al.ApJ, 997(1):31, Jan

    work page doi:10.1088/0004-637x/710/1/706

  60. [60]

    doi: 10.3847/1538-4357/ae1b93. M. C. Miller and D. P. Hamilton.MNRAS, 330(1):232–240, Feb

    work page doi:10.3847/1538-4357/ae1b93

  61. [61]

    2003.06918.x

    doi: 10.1046/j.1365-8711. 2002.05112.x. E. A. C. Mills et al.ApJ, 868(1):7, Nov

    work page doi:10.1046/j.1365-8711 2002

  62. [62]

    doi: 10.3847/1538-4357/aae581. K. Mori et al.ApJ, 921(2):148, Nov

    work page doi:10.3847/1538-4357/aae581

  63. [63]

    doi: 10.3847/1538-4357/ac1da5. M. Morris.ApJ, 408:496–506, May

    work page doi:10.3847/1538-4357/ac1da5

  64. [64]

    doi: 10.1086/172607. G. Nandakumar et al.MNRAS, 478:4374–4389, Aug

    work page doi:10.1086/172607

  65. [65]

    doi: 10.1093/mnras/sty1255. M. R. Nasirzadeh et al.A&A, 691:A199, Nov

    work page doi:10.1093/mnras/sty1255

  66. [66]

    23 The Galactic Centre Schödel et al

    doi: 10.1051/0004-6361/202451110. 23 The Galactic Centre Schödel et al. F. Nogueras-Lara et al.A&A, 631:A20, Nov

    work page doi:10.1051/0004-6361/202451110

  67. [67]

    F.Nogueras-Laraetal.NatureAstronomy,4:377–381,Jan.2020.doi: 10.1038/s41550-019-0967-9

    doi: 10.1051/0004-6361/201936263. F.Nogueras-Laraetal.NatureAstronomy,4:377–381,Jan.2020.doi: 10.1038/s41550-019-0967-9. F.Nogueras-Lara,R.Schödel,andN.Neumayer.NatureAstronomy,6:1178–1184,Aug.2022. doi: 10.1038/s41550-022-01755-3. T. Panamarev et al.MNRAS, 484(3):3279–3290, Apr

    work page doi:10.1051/0004-6361/201936263 2020

  68. [68]

    doi: 10.1093/mnras/stz208. F. Peißker et al.ApJ, 970(1):74, July

    work page doi:10.1093/mnras/stz208

  69. [69]

    doi: 10.3847/1538-4357/ad4098. O. Pfuhl et al.ApJ, 741:108, Nov

    work page doi:10.3847/1538-4357/ad4098

  70. [70]

    doi: 10.1088/0004-637X/741/2/108. G. Ponti et al.Nature, 567(7748):347–350, Mar

    work page doi:10.1088/0004-637x/741/2/108

  71. [71]

    doi: 10.1038/s41586-019-1009-6. G. Ponti et al.A&A, 646:A66, Feb

    work page doi:10.1038/s41586-019-1009-6

  72. [72]

    doi: 10.1051/0004-6361/202039636. S. F. Portegies Zwart and S. L. W. McMillan.ApJ, 576(2):899–907, Sept

    work page doi:10.1051/0004-6361/202039636

  73. [73]

    doi: 10.3847/0004-637X/818/2/

    work page doi:10.3847/0004-637x/818/2/

  74. [74]

    doi: 10.1051/0004-6361/202037800. M. J. Reid et al.ApJ, 783:130, Mar

    work page doi:10.1051/0004-6361/202037800

  75. [75]

    doi: 10.1088/0004-637X/783/2/130. M. A. Requena-Torres, J. Martín-Pintado, S. Martín, and M. R. Morris.ApJ, 672(1):352–360, Jan

    work page doi:10.1088/0004-637x/783/2/130

  76. [76]

    doi: 10.1086/523627. R. M. Rich et al.AJ, 154:239, Dec

    work page doi:10.1086/523627

  77. [77]

    doi: 10.3847/1538-3881/aa970a. V. M. Rivilla et al.MNRAS, 506(1):L79–L84, Sept

    work page doi:10.3847/1538-3881/aa970a

  78. [78]

    doi: 10.1093/mnrasl/slab074. V. M. Rivilla et al.ApJ, 929(1):L11, Apr

    work page doi:10.1093/mnrasl/slab074

  79. [79]

    doi: 10.3847/2041-8213/ac6186. V. M. Rivilla et al.ApJ, 953(2):L20, Aug

    work page doi:10.3847/2041-8213/ac6186 2041

  80. [80]

    doi: 10.3847/2041-8213/ace977. L. F. Rodríguez-Almeida et al.ApJ, 912(1):L11, May 2021a. doi: 10.3847/2041-8213/abf7cb. L. F. Rodríguez-Almeida et al.A&A, 654:L1, Oct. 2021b. doi: 10.1051/0004-6361/202141989. S. C. Rose, S. Naoz, R. Sari, and I. Linial.ApJ, 929(2):L22, Apr

    work page doi:10.3847/2041-8213/ace977 2041

Showing first 80 references.