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EVIDENCE FOR WARPED DISKS OF YOUNG STARS IN THE GALACTIC CENTER
Open accessAbstract
The central parsec around the supermassive black hole in the Galactic center (GC) hosts more than 100 young and massive stars. Outside the central cusp ( R ∼ 1'') the majority of these O and Wolf–Rayet (W–R) stars reside in a main clockwise system, plus a second, less prominent disk or streamer system at large angles with respect to the main system. Here we present the results from new observations of the GC with the AO-assisted near-infrared imager NACO and the integral field spectrograph SINFONI on the ESO/VLT. These include the detection of 27 new reliably measured W–R/O stars in the central 12'' and improved measurements of 63 previously detected stars, with proper motion uncertainties reduced by a factor of 4 compared to our earlier work. Based on the sample of 90 well measured W–R/O stars, we develop a detailed statistical analysis of their orbital properties and orientations. We show that half of the W–R/O stars are compatible with being members of a clockwise rotating system. The rotation axis of this system shows a strong transition from the inner to the outer regions as a function of the projected distance from Sgr A*. The main clockwise system either is either a strongly warped single disk with a thickness of about 10°, or consists of a series of streamers with significant radial variation in their orbital planes. Eleven out of 61 clockwise moving stars have an angular separation of more than 30° from the local angular momentum direction of the clockwise system. The mean eccentricity of the clockwise system is 0.36 ± 0.06. The distribution of the counterclockwise W–R/O star is not isotropic at the 98% confidence level. It is compatible with a coherent structure such as stellar filaments, streams, small clusters or possibly a disk in a dissolving state: 10 out of 29 counterclockwise moving W–R/O stars have an angular separation of more than 30° from the local angular momentum direction of the counterclockwise system. The observed disk warp and the steep surface density distribution favor in situ star formation in gaseous accretion disks as the origin of the young massive stars.
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“Additionally, the rotation vectors of individual stars within the clockwise system slightly vary from each other but, overall, remain at an inclination of 122 ◦ ± 7 ◦ (about ∼ 30 ◦ away from the Galactic rotation axis) (Paumard et al. 2006; Bartko et al. 2009; Lu et al. 2008; Genzel et al. 2010).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Bartko et al. 2009
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“A younger generation of stars (age ≈ 6 ± 2 Myr) is also observed within the central 0 . 5 pc (Paumard et al. 2006; Bartko et al. 2009).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Bartko et al. 2009
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MONITORING STELLAR ORBITS AROUND THE MASSIVE BLACK HOLE IN THE GALACTIC CENTER
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A star in a 15.2-year orbit around the supermassive black hole at the centre of the Milky Way
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“It is associated with the compact radio source Sgr A*, which must be a massive black hole, beyond any reasonable doubt (Schödel et al. 2002; Ghez et al. 2005; Gillessen et al. 2009).”
Self-citationEvidence for a black hole from high rotation velocities in a sub-parsec region of NGC4258
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“It is also interesting to note a well known example of another warped nuclear disk surrounding a supermassive black hole in another galaxy; the maser disk observation of NGC 4258 (Miyoshi et al. 1995; Herrnstein et al. 1996).”
A new calibration of stellar parameters of Galactic O stars
Martins, F., Schaerer, D., & Hillier, D. J. (2005) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20042386 · Cited by 1,120 · cited 1×
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Self-citationTHE GALACTIC CENTER ENVIRONMENT
Morris, M., & Serabyn, E. (1996) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev.astro.34.1.645 · Cited by 930 · cited 1×
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The Proper Motion of Sagittarius A*. II. The Mass of Sagittarius A*
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Cited by
Sorted by citations
Items 101–200 of 281
The nuclear cluster of the Milky Way: total mass and luminosity
Fritz, T. K., Chatzopoulos, S., Gerhard, O., Gillessen, S., Genzel, R., Pfuhl, O., Tacchella, S., Eisenhauer, F., & Ott, T. (2013) · reroDoc Digital Library · doi:10.3929/ethz-b-000422972 · Cited by 56
Self-citationMisaligned streamers around a Galactic Centre black hole from a single cloud's infall
Lucas, W. E., Bonnell, I. A., Davies, M. B., & Rice, K. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt727 · Cited by 44
“5 C O N C L U S I O N S Recent observations indicate the presence of two misaligned discs of massive stars around Sagittarius A* (Paumard et al. 2006; Bartko et al. 2009).”
BackgroundInfluential0 The High-Density Ionized Gas in the Central Parsec of the GalaxyPreprint
Zhao, J., Blundell, R., Moran, J. M., Downes, D., Schuster, K.-F., & Marrone, D. P. (2010) · Cited by 46
Hydrodynamical simulations of a compact source scenario for the galactic center cloud G2
Ballone, A., Schartmann, M., Burkert, A. M., Gillessen, S., Genzel, R., Fritz, T. K., Eisenhauer, F., Pfuhl, O., & Ott, T. (2013) · Max Planck Digital Library · Cited by 44
Self-citationConstraining the initial mass function of stars in the Galactic Centre
Löckmann, U., Baumgardt, H., & Kroupa, P. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15906.x · Cited by 44
“Based on more recent spectroscopic observations, Bartko et al. (2009b) find strong evidence for this to be true.”
BackgroundInfluentialOn the origins of enigmatic stellar populations in Local Group galactic nuclei
Leigh, N. W. C., Antonini, F., Stone, N. C., Shara, M. M., & Merritt, D. R. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2018 · Cited by 42
“There exists tentative evidence for a second, less-massive and counterclockwise disk that consists of stars similar in their photometric, spectroscopic and even kinematic properties (e.g. Paumard et al. 2006; Bartko et al. 2009, 2010).”
BackgroundInfluentialAlfaro-Cuello, M., Kacharov, N., Neumayer, N., Bianchini, P., Mastrobuono-Battisti, A., Lützgendorf, N., Seth, A. C., Böker, T., Kamann, S., Leaman, R., et al. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab77bb · Cited by 43
“A representative case of a young stellar disk is observed in the Milky Way NSC (Genzel et al. 2003; Paumard et al. 2006; Bartko et al. 2009; Lu et al. 2009, 2013; Yelda et al. 2014; Feldmeier-Krause et al. 2015).”
BackgroundCONSTRAINING THE DARK CUSP IN THE GALACTIC CENTER BY LONG-PERIOD BINARIES
Tal Alexander, A., & Pfuhl, O. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/780/2/148 · Cited by 42
“IRS 16NE is a member of the clock-wise disk, a product of the recent starburst episode, whose age is estimated at T = (6 ± 2) × 106 yr (Paumard et al. 2006; Bartko et al. 2009; but see also younger age estimate by Lu et al. 2013).”
Self-citationThe Post-pericenter Evolution of the Galactic Center Source G2
Plewa, P. M., Gillessen, S., Pfuhl, O., Eisenhauer, F., Genzel, R., Burkert, A. M., Dexter, J., Habibi, M., George, E. M., Ott, T., et al. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa6e00 · Cited by 39
“The angular offset between the orientation of G2ʼs orbital plane and that of the clockwise stellar disk amounts to30° (Figure 6), while the apocenter of G2 at about1 projected distance from SgrA* still falls within the inner disk region (Paumard et al. 2006; Bartko et al. 2009; Yelda et al. 2014).”
BackgroundSelf-citationConfusing Binaries: The Role of Stellar Binaries in Biasing Disk Properties in the Galactic Center
Naoz, S., Ghez, A. M., Hees, A., Do, T., Witzel, G., & Lu, J. R. (2018) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/aaa6bf · Cited by 39
“The stellar membership estimations and the modeling of the disk’s properties are based on multiple years of astrometric measurements, but typically only use one radial velocity (Vz) measurement (e.g., Bartko et al. 2009; Yelda et al. 2014).”
BackgroundMethodResultInfluentialYoung, massive star candidates detected throughout the nuclear star cluster of the Milky Way
Nishiyama, S., & Schödel, R. (2012) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201219773 · Cited by 38
“This power-law agrees within t e uncertainties with the power-law that describes the surface density of correspondingly bright young stars withinR = 0.5 pc of Sgr A*, that were identified in spectroscopic studies (e.g., Bartko et al. 2009).”
BackgroundInfluentialDynamical constraints on the origin of the young B-stars in the Galactic center
Perets, H., & Gualandris, A. (2010) · Surrey Research Insight Open Access (The University of Surrey) · Cited by 38
Self-citationBinaries migrating in a gaseous disk: Where are the galactic center binaries?
Baruteau, C., Cuadra, J., & Lin, D. (2011) · Max Planck Digital Library · Cited by 38
Trani, A. A., Fujii, M. S., & Spera, M. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab0e70 · Cited by 37
Broderick, A. E., Fish, V. L., Johnson, M. D., Rosenfeld, K., Wang, C., Akiyama, K., Johannsen, T., Roy, A. L., & Doeleman, S. S. (2015) · DSpace@MIT (Massachusetts Institute of Technology) · Cited by 37
Isotropic–Nematic Phase Transitions in Gravitational Systems
Roupas, Z., Kocsis, B., & Tremaine, S. D. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa7141 · Cited by 40
“…density of various stellar types in NSCs increases steeply inwards with radius as r 1.5- to r 2.9- within the radius of influence of the SMBH, which is 1 pc~ for the NSC at the center of the Milky Way (Bartko et al. 2009; Schödel et al. 2009, 2014; Yelda et al. 2014; Chatzopoulos et al. 2015).”
BackgroundInfluentialRose, S. C., Naoz, S., Gautam, A. K., Ghez, A. M., Do, T., Chu, D., & Becklin, E. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abc557 · Cited by 41
THE FRAGMENTING PAST OF THE DISK AT THE GALACTIC CENTER: THE CULPRIT FOR THE MISSING RED GIANTS
Amaro‐Seoane, P., & Chen, X. (2014) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/781/1/l18 · Cited by 35
“However, the existence of this second disk is still in debate (Paumard et al. 2006; Lu et al. 2006; Bartko et al. 2009).”
BackgroundMassive binaries in the vicinity of Sgr A
Pfuhl, O., Tal Alexander, A., Gillessen, S., Martins, F., Genzel, R., Eisenhauer, F., Fritz, T. K., & Ott, T. (2013) · HAL · Cited by 35
Self-citationThe mass function of nearby black hole candidates
Caramete, L., & Biermann, P. L. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200913146 · Cited by 35
“However, including the process of massive star formation, e.g.,(Bartko et al. 2009) near the center of a galaxy might require a certain minimum amount of gaseous turn-over by star (star formation, mass ejection by winds, and explosions), and so it is conceivable that these processes define a…”
BackgroundThe Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way
Sarkar, K. C. (2024) · The Astronomy and Astrophysics Review · doi:10.1007/s00159-024-00152-1 · Cited by 34
ON THE ORIGIN OF THE B-STARS IN THE GALACTIC CENTER
Madigan, A.-M., Pfuhl, O., Levin, Y., Gillessen, S., Genzel, R., & Perets, H. B. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/784/1/23 · Cited by 39
“′′8–12′′ (Levin & Beloborodov 2003; Genzel et al. 2003; Lu et al. 2009; Bartko et al. 2009), although more young star candidates have been detected at larger distances (Bartko et al. 2010; Nishiyama & Schödel 2013).”
BackgroundMethodInfluentialSelf-citationApproaching hell’s kitchen: Molecular daredevil clouds in the vicinity of Sagittarius A*
Moser, L., Sánchez-Monge, Á., Eckart, A., Requena-Torres, M. A., García-Marin, M., Kunneriath, D., Zensus, A., Britzen, S., Sabha, N., Shahzamanian, B., et al. (2017) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201628385 · Cited by 34
“LMoser_GC-ALMA_final (∼ 6×106 yr; Paumard et al. 2006; Bartko et al. 2009) of many of these stars suggests they formed in situ and challenges our current understanding of star formation in such environments (e.g., Nayakshin et al. 2007).”
BackgroundInfluentialThe fragmenting past of the disk at the Galactic Center : The culprit for the missing red giants
Amaro‐Seoane, P., & Chen, X. (2014) · MPG.PuRe (Max Planck Society) · Cited by 34
Jia, S., Lu, J. R., Sakai, S., Gautam, A. K., Do, T., Hosek, M. W., Service, M., Ghez, A. M., Gallego-Cano, E., Schödel, R., et al. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab01de · Cited by 37
“…et al. 2010), (2) the formation mechanism of the young populations is still not well understood (Levin & Beloborodov 2003; Nayakshin & Sunyaev 2005; Bartko et al. 2009; Lu et al. 2009), (3) there are many unusual stars that may be the product of tidal interactions with the SMBH or with other stars…”
BackgroundInfluentialKim, J., Marrone, D. P., Chan, C.-K., Medeiros, L., Özel, F., & Psaltis, D. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/832/2/156 · Cited by 32
“…at many baselines as well as sets of closure phases on baseline 4 Another often used angle to measure the same orientation is denoted by φ and is the complementary angle to ξ, measured in degrees north of east (e.g., Bartko et al. 2009); clearly, ξ = 90◦−φ. 3 triangles and closure amplitudes.”
BackgroundKaaz, N., Schrøder, S. L., Andrews, J. J., Antoni, A., & Ramirez-Ruiz, E. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/aca967 · Cited by 32
The X-Ray Binary Population in the Galactic Center Revealed through Multi-decade Observations
Mori, K., Hailey, C. J., Schutt, T., Mandel, S., Heuer, K., Grindlay, J. E., Hong, J., Ponti, G., & Tomsick, J. A. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/ac1da5 · Cited by 32
Fragione, G., & Antonini, F. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz1723 · Cited by 32
“Even though the star-formation rate close to non-resolved regions around SMBHs is difficult to estimate, we use an empirical estimate based on our Galactic Centre (see e.g. Bartko et al. 2009).”
MethodApproaching hell’s kitchen: Molecular daredevil clouds in the vicinity of Sagittarius A*
Moser, L., Sánchez-Monge, Á., Eckart, A., Requena-Torres, M. A., García-Marín, M., Kunneriath, D., Zensus, J. A., Britzen, S., Sabha, N. B., Shahzamanian, B., et al. (2017) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201628385/pdf · Cited by 31
Where intermediate-mass black holes could hide in the Galactic Centre
Straub, O., Bauböck, M., Abuter, R., Aimar, N., Amaro‐Seoane, P., Amorim, A., Berger, J.-P., Bonnet, H., Bourdarot, G. G., Brandner, W., et al. (2023) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202245132 · Cited by 31
Self-citationSelf-gravitating warped discs around supermassive black holes
Ulubay-Siddiki, A., Gerhard, O., & Arnaboldi, M. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15089.x · Cited by 31
“Of the ∼100 massive young stars in the centre of our Galaxy about half form a well-defined, warped disc, and some of the others are on a counterrotating structure which may be a dissolving disc (Genzel et al. 2003; Paumard et al. 2006; Bartko et al. 2009; Lu et al. 2009).”
BackgroundInfluentialSelf-citationON THE EXISTENCE OF PULSARS IN THE VICINITY OF THE MASSIVE BLACK HOLE IN THE GALACTIC CENTER
Zhang, F., Lu, Y., & Yu, Q. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/784/2/106 · Cited by 31
“…2010, and Zhang et al. 2010) find that the current observations on both the GC Sstars and the HVSs are compatible with the model that their progenitorial stellar binaries are originated from the young stellar disk(s) at a distance of 0.04 − 0.5 pc from the MBH (Lu et al. 2009; Bartko et al. 2009).”
ResultInfluentialMASSIVE STAR FORMATION OF THE SGR A EAST H II REGIONS NEAR THE GALACTIC CENTER
Yusef-Zadeh, F., Lacy, J. H., Wardle, M., Whitney, B. A., Bushouse, H., Roberts, D. A., & Arendt, R. G. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/725/2/1429 · Cited by 30
“This has the ramification that the formation of massive stellar clusters must be pervasive in this region as evidenced by the Arches and Quintuple clusters as well as the nuclear massive cluster centered on Sgr A* (Figer et al. 2002; Bartko et al. 2009, and the references therein).”
BackgroundCan supernova kicks trigger EMRIs in the Galactic Centre?
Bortolas, E., & Mapelli, M. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz440 · Cited by 30
“…≈ 4.3× 106 M (Schödel et al. 2002; Ghez et al. 2003; Gillessen et al. 2017), and several hundreds of young massive stars (including WolfRayet stars and O- and B-type stars) have been spotted within the innermost 0.5 pc (Paumard et al. 2006; Bartko et al. 2009; Do et al. 2013; Yelda et al. 2014).”
BackgroundInfluentialJia, S., Lu, Jr., Sakai, S., Gautam, A., Do, T., Hosek, M., Service, M., Ghez, A., Gallego-Cano, E., Schödel, R., et al. (2019) · eScholarship (California Digital Library) · Cited by 30
Evidence for a jet and outflow from Sgr A*: a continuum and spectral line study
Yusef-Zadeh, F., Royster, M., Wardle, M., Cotton, W., Kunneriath, D., Heywood, I., & Michail, J. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa2399 · Cited by 31
“The orbits of most of these stars lie in the “clockwise disk” , with orbital planes distributed around a mean PA of their ascending nodes Ω ≈ 106◦ E of N and mean inclination i ≈ 126◦ to the line of sight (Bartko et al. 2009; Gillessen et al. 2009; Yelda et al. 2014; Gillessen et al. 2017).”
BackgroundTHE SPATIAL AND VELOCITY DISTRIBUTIONS OF HYPERVELOCITY STARS
Zhang, F., Lu, Y., & Yu, Q. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/722/2/1744 · Cited by 29
“…the same as that of CWS disk located within half a parsec from the central MBH (see Levin & Beloborodov 2003; Lu et al. 2009; Paumard et al. 2006; Bartko et al. 2009, 2010); (2) four of the unbound HVSs (plus three bound ones and two candidates; totally 9 objects) are spatially associated to a…”
BackgroundAbbate, F., Mastrobuono-Battisti, A., Colpi, M., Possenti, A., Sippel, A. C., & Dotti, M. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx2364 · Cited by 29
“In the in-situ formation scenario, ordinary pulsars form out of regular star formation and should be found where young massive stars are observed, ∼ 0.5 pc (Bartko et al. 2009; Yusef-Zadeh et al. 2013; Mapelli & Gualandris 2016).”
BackgroundInfluentialAn Adaptive Optics Survey of Stellar Variability at the Galactic Center
Gautam, A. K., Do, T., Ghez, A. M., Morris, M. R., Martinez, G. D., Hosek, M. W., Lu, J. R., Sakai, S., Witzel, G., Jia, S., et al. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/aaf103 · Cited by 27
“This sample of stars was further subdivided into known early- and late-type stars (identified by Paumard et al. 2006; Bartko et al. 2009; Do et al. 2009, 2012; Gillessen et al. 2009, and manually assigned a spectral type according to Do et al. 2013a).”
BackgroundCAN STAR–DISK COLLISIONS EXPLAIN THE MISSING RED GIANTS PROBLEM IN THE GALACTIC CENTER?
Kieffer, T. F., & Bogdanović, T. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/823/2/155 · Cited by 26
“This hypothesis is motivated by the observational evidence for a disk of early-type stars surrounding the SMBH and extending from approximately 0.04 pc out to 0.5 pc (Paumard et al. 2006; Lu et al. 2009; Bartko et al. 2009; Støstad et al. 2015).”
BackgroundMethodInfluentialŠubr, L., & Haas, J. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/828/1/1 · Cited by 26
“0.4 pc from the SMBH (e.g. Paumard et al. 2006; Bartko et al. 2009, 2010; Do et al. 2013).”
InfluentialProperties of bow-shock sources at the Galactic center
Sánchez-Bermúdez, J., Schödel, R., Alberdi, A., Mužić, K., Hummel, C. A., & Pott, J. (2014) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201423657/pdf · Cited by 24
Modelling the formation of the circumnuclear ring in the Galactic centre
Mapelli, M., & Trani, A. A. (2015) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201527195 · Cited by 25
“About 20% of them lie in a ring that has an outer radius ∼0.15 pc, named the clockwise (CW) disc for its orientation when projected on the plane of the sky (Paumard et al. 2006; Bartko et al. 2009; Lu et al. 2009, 2013; Yelda et al. 2014).”
BackgroundInfluentialProperties of bow-shock sources at the Galactic center
Sánchez-Bermúdez, J., Schödel, R., Alberdi, A., Muzić, K., Hummel, C. A., & Pott, J.-U. (2014) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201423657 · Cited by 27
“…along with the finding that the young stars are concentrated toward the black hole, gave rise to the currently favored hypothesis for their formation in situ in a formerly existing gas disk around Sagittarius A* (Levin & Beloborodov 2003; Paumard et al. 2006; Lu et al. 2009; Bartko et al. 2009).”
BackgroundGalactic Center IRS 13E: Colliding Stellar Winds or an Intermediate-mass Black Hole?
Zhu, Z., Li, Z., Ciurlo, A., Morris, M. R., Zhang, M., Do, T., & Ghez, A. M. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab980d · Cited by 25
The episodic and multiscale Galactic Centre
Bryant, A., & Krabbe, A. (2021) · New Astronomy Reviews · doi:10.1016/j.newar.2021.101630 · Cited by 29
Three-body encounters in black hole discs around a supermassive black hole
Trani, A. A., Quaini, S., & Colpi, M. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202347920 · Cited by 25
JASMINE: Near-infrared astrometry and time-series photometry science
Kawata, D., Kawahara, H., Gouda, N., Secrest, N. J., Kano, R., Kataza, H., Isobe, N., Ohsawa, R., Usui, F., Yamada, Y., et al. (2024) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psae020 · Cited by 35
Self-citationStar Formation and Dynamics in the Galactic Centre
Mapelli, M., & Gualandris, A. (2015) · Lecture notes in physics · doi:10.1007/978-3-319-19416-5_6 · Cited by 26
“This is the reason why previous studies proposed that the CNR formed through the collision of twomolecular clouds 18 Michela Mapelli and Alessia Gualandris (e.g. Guesten et al. 1987) or through the assembly of multiple dynamically different streamers (e.g. Jackson et al. 1993).”
BackgroundMethodResultInfluentialAn Adaptive Optics Survey of Stellar Variability at the Galactic Center
Gautam, A. K., Do, T., Ghez, A. M., Morris, M., Martinez, G. D., Hosek, M. W., Lu, J. R., Sakai, S., Witzel, G., Jia, S., et al. (2019) · eScholarship (California Digital Library) · Cited by 24
Secular theory of the orbital evolution of the young stellar disc in the Galactic Centre
Haas, J., Šubr, L., & Vokrouhlický, D. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.19100.x · Cited by 24
“Observations suggest that about one half of them form a coherently rotating disc-like structure with estimated surface density profile Σ ∝ R−2 (Paumard et al. 2006; Lu et al. 2009; Bartko et al. 2009) which implies the above considered distribution of semi-major axes.”
BackgroundMethodIsotropic–Nematic Phase Transitions in Gravitational Systems. II. Higher Order Multipoles
Takács, Á., & Kocsis, B. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aab268 · Cited by 23
“It may have applications in explaining the origin of a thin disk of massive stars in the Galactic center (Bartko et al. 2009; Kocsis & Tremaine 2011; Haas & Šubr 2014a, 2014b; Yelda et al. 2014; Panamarev et al. 2018; Perets et al. 2018) and the distribution of possible putative stellar mass black…”
BackgroundTWO-BODY RELAXATION DRIVEN EVOLUTION OF THE YOUNG STELLAR DISK IN THE GALACTIC CENTER
Šubr, L., & Haas, J. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/786/2/121 · Cited by 23
“…and techniques in the past few decades, however, led to a surprising discovery of a significant number of young stars in the innermost parsec of the Galaxy (e.g. Paumard et al. 2006; Bartko et al. 2009, 2010; Do et al. 2013) which appear to be orbiting the central SMBH on near-Keplerian orbits.”
High-redshift SMBHs can grow from stellar-mass seeds via chaotic accretion
Zubovas, K., & King, A. R. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab004 · Cited by 23
Schartmann, M., Ballone, A., Burkert, A. M., Gillessen, S., Genzel, R., Pfuhl, O., Eisenhauer, F., Plewa, P. M., Ott, T., George, E. M., et al. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/811/2/155 · Cited by 22
“The latter are made up of roughly 100 massive O- and Wolf- Rayet stars distributed in a warped clockwise rotating disk ranging from roughly 0.05 to around 0.5 pc (Paumard et al. 2006; Bartko et al. 2009; Lu et al. 2009; Yelda et al. 2014).”
BackgroundInfluentialSelf-citationGualandris, A., Mapelli, M., & Perets, H. B. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.22133.x · Cited by 22
“Bartko et al. (2009) perform a statistical analysis of the candidate disc members, assuming Keplerian orbits in the gravitational potential of the SMBH and the stellar cusp, and derive distributions for the orbital elements of the stars.”
BackgroundMethodResultInfluentialSelf-citationStellar Populations in the Central 0.5 pc of Our Galaxy. III. The Dynamical Substructures
Jia, S., Xu, N., Lu, J. R., Chu, D. S., O’Neil, K. K., Drechsler, W. B., Hosek, M. W., Sakai, S., Do, T., Ciurlo, A., et al. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acb939 · Cited by 22
The coupling of a young stellar disc with the molecular torus in the Galactic Centre
Haas, J., Šubr, L., & Kroupa, P. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.18025.x · Cited by 21
“The observations suggest that all the WR/OB stars have mass m & 12M⊙ (Paumard et al. 2006; Bartko et al. 2009, 2010).”
BackgroundResultInfluentialColliding winds in and around the stellar group IRS 13E at the galactic centre
Wang, Q. D., Li, J., Russell, C. M. P., & Cuadra, J. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz3624 · Cited by 23
Nobel Lecture: A forty-year journey
Genzel, R. (2022) · Reviews of Modern Physics · doi:10.1103/revmodphys.94.020501 · Cited by 23
Self-citationHypervelocity Stars Track Back to the Galactic Center in Gaia DR3
Liao, J., Du, C., Li, H., Ma, J., & Shi, J. (2023) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/acb7d9 · Cited by 21
Star formation at the Galactic Centre: coevolution of multiple young stellar discs
Mastrobuono-Battisti, A., Perets, H. B., Gualandris, A., Neumayer, N., & Sippel, A. C. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz3004 · Cited by 22
“The presence of a second counter-clockwise and approximately coeval disc is still debated (Genzel et al. 2003; Paumard et al. 2006; Bartko et al. 2009; Lu et al. 2009, 2013).”
BackgroundInfluentialSelf-citationIsotropic-Nematic Phase Transitions in Gravitational Systems. II. Higher Order Multipoles
Takács, Á., & Kocsis, B. (2018) · Repository of the Academy's Library (Library of the Hungarian Academy of Sciences) · Cited by 20
Trani, A. A., Mapelli, M., & Ballone, A. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aad414 · Cited by 20
Peißker, F., Eckart, A., Sabha, N. B., Zajaček, M., & Bhat, H. K. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab9826 · Cited by 20
“In terms of stellar populations, the Brγ bar can be found at larger scales than the S-cluster (1′′ ∼ 0.04 pc), potentially within the Clockwise Disk (CWD) of young massive OB stars located between 0.032 − 0.48 pc (Bartko et al. 2009).”
BackgroundInfluentialPerturbations induced by a molecular cloud on the young stellar disc in the Galactic Centre
Mapelli, M., Gualandris, A., & Hayfield, T. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt1858 · Cited by 19
“This value is consistent with most observations (e.g. Paumard et al. 2006; Bartko et al. 2009), but is a factor of ∼3 lower than the most recent results (Lu et al. 2013).”
BackgroundResultInfluentialHot molecular hydrogen in the central parsec of the Galaxy through near-infrared 3D fitting
Ciurlo, A., Paumard, T., Rouan, D., & Clénet, Y. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201527173 · Cited by 19
“We have completed the calibration using stars in the field chosen from the catalogs of Paumard et al. (2006), Blum et al. (2003), and Bartko et al. (2009).”
MethodSelf-citationOn the origin of the B-stars in the galactic center
Madigan, A., Pfuhl, O., Levin, Y., Gillessen, S., Genzel, R., & Perets, H. (2014) · Max Planck Digital Library · Cited by 19
Self-citationGoing with the flow: using gas clouds to probe the accretion flow feeding Sgr A*
McCourt, M., & Madigan, A.-M. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2232 · Cited by 18
“In figure 8, we also mark the position of the (inner edge of the) clockwise disk with red error bars (Bartko et al. 2009; Lu et al. 2009).”
BackgroundEvans, F. A., Rasskazov, A., Remmelzwaal, A., Marchetti, T., Castro-Ginard, A., Rossi, E. M., & Bovy, J. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad2273 · Cited by 23
Counter-rotating stellar discs around a massive black hole: self-consistent, time-dependent dynamics
Touma, J., & Sridhar, S. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.21000.x · Cited by 17
“The remaining young stars appear to be members of a counter-rotating population which is thicker than and inclined to the warped disc (Genzel et al. 2003; Paumard et al. 2006; Bartko et al. 2009, 2010).”
Hamers, A. S., & Perets, H. B. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa7f29 · Cited by 19
“In the GC in particular, such processes may have contributed to the formation of the innermost O stars, which are concentrated in a disk-like structure (e.g., Genzel et al. 2000; Levin & Beloborodov 2003; Paumard et al. 2006; Tanner et al. 2006; Bartko et al. 2009; Lu et al. 2009).”
BackgroundSelf-citationA numerical study of stellar discs in galactic nuclei
Panamarev, T., & Kocsis, B. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3050 · Cited by 20
SIGNATURES OF PLANETS AND PROTOPLANETS IN THE GALACTIC CENTER: A CLUE TO UNDERSTANDING THE G2 CLOUD?
Mapelli, M., & Ripamonti, E. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/806/2/197 · Cited by 17
“…dense star cluster of old stars (Schödel et al. 2007), several thousand solar masses of molecular, atomic and ionized gas (Liu et al. 2012; Jackson et al. 1993; Scoville et al. 2003), and a few hundred young stars (Genzel et al. 2003; Paumard et al. 2006; Bartko et al. 2009; Lu et al. 2009, 2013).”
BackgroundInfluentialMisaligned Jets from Sgr A* and the Origin of Fermi/eROSITA Bubbles
Sarkar, K. C., Mondal, S., Sharma, P., & Piran, T. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acd75d · Cited by 17
Gautam, A. K., Do, T., Ghez, A. M., Chu, D. S., Hosek, M. W., Sakai, S., Naoz, S., Morris, M., Ciurlo, A., Haggard, Z., et al. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad26e6 · Cited by 16
Mapping the Galactic centre’s dark cluster via resonant relaxation
Tep, K., Fouvry, J.-B., Pichon, C., Heißel, G., Paumard, T., Perrin, G. S., & Vincent, F. H. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab1945 · Cited by 16
Self-citationThe Apparent Tail of the Galactic Center Object G2/DSO
Peißker, F., Zajaček, M., Eckart, A., Ali, B., Karas, V., Sabha, N. B., Grellmann, R., Labadie, L., & Shahzamanian, B. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/ac23df · Cited by 16
Are supermassive black holes shrouded by ‘super-Oort’ clouds of comets and asteroids?
Nayakshin, S., Sazonov, S., & Sunyaev, R. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.19777.x · Cited by 15
“At the same time we know that there was a star formation event ∼ 6 Myr ago, with the total stellar mass less than Mt ∼ 10 4 M⊙ (Paumard et al. 2006), and that the geometrical arrangement of the stars is far from flat (Bartko et al. 2009).”
BackgroundSelf-citationDYNAMICS OF TIDALLY CAPTURED PLANETS IN THE GALACTIC CENTER
Trani, A. A., Mapelli, M., Spera, M., & Bressan, A. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/831/1/61 · Cited by 15
“…Myr) stars (mainly Wolf-Rayet and O-type stars, Paumard et al. 2006; Lu et al. 2009, 2013) lie further out (> 0.04 pc), 20% of which form a nearly-Keplerian disk around the SMBH, named clockwise (CW) disk for its motion when projected on the plane of the sky (Bartko et al. 2009; Yelda et al. 2014).”
BackgroundInfluentialDong, H., Schödel, R., Williams, B. F., Nogueras-Lara, F., Gallego-Cano, E., Gallego-Calvente, A. T., Wang, Q. D., Morris, M., Do, T., & Ghez, A. M. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx1436 · Cited by 14
“In total, Paumard et al. (2006), Bartko et al. (2009) and Feldmeier-Krause et al. (2015) identify (or tentatively classify) 153 WR stars, OB supergiants and main-sequence stars.”
BackgroundResultOrbital alignment and mass segregation in galactic nuclei via vector resonant relaxation
Magnan, N., Fouvry, J.-B., Pichon, C., & Chavanis, P.-H. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac1248 · Cited by 16
The evolution of circumstellar discs in the galactic centre: an application to the G-clouds
Owen, J. E., & Lin, D. N. C. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3506 · Cited by 16
ORIGIN OF THE GALACTIC CENTER S-STARS: GRAVITATIONAL TORQUES FROM LIN-SHU-TYPE SPIRAL DENSITY WAVES
Griv, E. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/709/2/597 · Cited by 14
Random forest classification of stars in the Galactic Centre
Plewa, P. M. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty511 · Cited by 15
“A significant fraction of the most massive young (WR/O-)stars reside in a disc structure (Paumard et al. 2006; Lu et al. 2009; Bartko et al. 2009; Yelda et al. 2014), while an apparently isotropically distributed “S-star” cluster of less massive (B-)stars is concentrated around the central massive…”
BackgroundMethodResultGRAVITY: Astrometry on the galactic center and beyond
Bartko, H., Perrin, G. S., Brandner, W., Straubmeier, C., Richichi, A., Gillessen, S., Paumard, T., Hippler, S., Eckart, A., Schöller, M., et al. (2009) · New Astronomy Reviews · doi:10.1016/j.newar.2010.07.002 · Cited by 14
Self-citationTHE BLACK HOLE MASS AND THE STELLAR RING IN NGC 3706
Gültekin, K., Gebhardt, K., Kormendy, J., Lauer, T. R., Bender, R., Tremaine, S. D., & Richstone, D. O. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/781/2/112 · Cited by 13
“At even smaller scales, within ∼ 0.5 pc of the Galactic center, there appear to be two young stellar disks that rotate in different directions (Levin & Beloborodov 2003; Paumard et al. 2006; Lu et al. 2009; Bartko et al. 2009).”
BackgroundInfluentialEnhanced Extreme Mass Ratio Inspiral Rates and Intermediate Mass Black Holes
Qunbar, I., & Stone, N. C. (2024) · Physical Review Letters · doi:10.1103/physrevlett.133.141401 · Cited by 13
THE HISTORY OF TIDAL DISRUPTION EVENTS IN GALACTIC NUCLEI
Aharon, D., Mastrobuono-Battisti, A., & Perets, H. B. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/823/2/137 · Cited by 13
“For both of the scenarios, The chosen slope of the SF function is motivated by the observed power-law (Do et al. 2009; Bartko et al. 2009) distribution of young stars observed in the young stellar disk in the GC.”
BackgroundSelf-citationLeaman, R., & van de Ven, G. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab1966 · Cited by 16
Spectroscopically identified intermediate age stars at 0.5–3 pc distance from Sagittarius A*
Nishiyama, S., Schödel, R., Yoshikawa, T., Nagata, T., Minowa, Y., & Tamura, M. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201322392 · Cited by 13
“…at the center of the Milky Way’s NSC, within a projected distance of about 0.5 pc of the SMBH Sagittarius A* (Sgr A*), was identified by spectroscopic observations and traces a starburst that occurred a few Myr ago (e.g., Paumard et al. 2006; Bartko et al. 2009; Lu et al. 2013; Yelda et al. 2014).”
BackgroundInfluentialSgr A* envelope explosion and the young stars in the centre of the Milky Way
Nayakshin, S., & Zubovas, K. (2018) · Monthly Notices of the Royal Astronomical Society: Letters · doi:10.1093/mnrasl/sly082 · Cited by 12
“The observed population is not as numerous or eccentric (Bartko et al. 2009).”
BackgroundSelf-citationTHE INFLUENCE OF DENSE GAS RINGS ON THE DYNAMICS OF A STELLAR DISK IN THE GALACTIC CENTER
Trani, A. A., Mapelli, M., Bressan, A., Pelupessy, F. I., van Elteren, A., & Zwart, S. P. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/818/1/29 · Cited by 12
“Some of these stars lie in a near-Keplerian disk, called clockwise (CW) disk from the motion that it shows when projected on the plane of the sky (Paumard et al. 2006; Lu et al. 2009; Bartko et al. 2009; Do et al. 2013; Lu et al. 2013; Yelda et al. 2014).”
InfluentialSecular Evolution Driven by Massive Eccentric Disks/Rings: An Apsidally Aligned Case
Davydenkova, I., & Rafikov, R. R. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aad3ba · Cited by 12
“Our own Galaxy harbors an eccentric disk of young stars orbiting the central supermassive black hole (Levin & Beloborodov 2003; Bartko et al. 2009), whose gravity may affect its own dynamics (Nayakshin et al. 2006).”
BackgroundSpectroscopically identified intermediate age stars at 0.5–3 pc distance from Sagittarius A*
Nishiyama, S., Schödel, R., Yoshikawa, T., Nagata, T., Minowa, Y., & Tamura, M. (2016) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201322392/pdf · Cited by 12
van Donkelaar, F., Mayer, L., Capelo, P. R., Tamfal, T., Quinn, T., & Madau, P. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae804 · Cited by 11
Globular cluster ejection, infall, and the host dark matter halo of the Pegasus dwarf galaxy
Leaman, R., Ruiz-Lara, T., Cole, A. A., Beasley, M. A., Boecker, A., Fahrion, K., Bianchini, P., Falcón‐Barroso, J., Webb, J. J., Sills, A., et al. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa004 · Cited by 11
The quenching of star formation in accretion-driven clumpy turbulent tori of active galactic nuclei
Vollmer, B., & Davies, R. (2013) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201321409 · Cited by 11
“This might help to explain the paradox of youth (Ghez et al. 2003), i.e. the lack of young massive stars at galactic radii> 0.5 pc and the relatively low eccentricities of these stars within the central parsec of the Galaxy (Bartko et al. 2009).”
BackgroundInfluentialAre supermassive black holes shrouded by 'super-Oort' clouds of comets and asteroids?
(7603817), S. S., & (7603820), R. S. (2012) · Figshare · Cited by 11
Metadata
- Authors
- Bartko, H., Martins, F., Fritz, T. K., Genzel, R., Levin, Y., Perets, H. B., Paumard, T., Nayakshin, S., Gerhard, O., Alexander, T., Dodds-Eden, K., Eisenhauer, F., Gillessen, S., Mascetti, L., Ott, T., Perrin, G., Pfuhl, O., Reid, M. J., Rouan, D., Sternberg, A., & Trippe, S.
- Affiliations
- Max Planck Institute for Extraterrestrial Physics (DE)
- Centre National de la Recherche Scientifique (FR)
- Leiden University (NL)
- Weizmann Institute of Science (IL)
- University of Leicester (GB)
- Harvard University (US)
- Tel Aviv University (IL)
- Corresponding author
- Bartko, H.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2009-05-14
- Volume
- 697
- Issue
- 2
- Pages
- 1741-1763
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2002943556
- Cited by
- 282
- References
- 86
- Citations by year
- 2026: 10 · 2025: 11 · 2024: 12 · 2023: 15 · 2022: 9 · 2021: 11 · 2020: 16 · 2019: 18 · 2018: 19 · 2017: 17 · 2016: 21 · 2015: 16 · 2014: 25 · 2013: 24 · 2012: 18
- FWCI
- 9.73
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- The Astrophysical Journal (publishedVersion)
- HAL (submittedVersion)
- arXiv (Cornell University) (submittedVersion)
- Leiden Repository (Leiden University) (submittedVersion)
- Data Archiving and Networked Services (DANS) (submittedVersion, other-oa)
- Max Planck Institute for Plasma Physics (submittedVersion)
- Leicester Research Archive (University of Leicester) (submittedVersion)
- arXiv (Cornell University)
- Funders
- Israel Science Foundation
- Science and Technology Facilities Council (PP/E00119X/1)
- FP7 Ideas: European Research Council (202996)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Keywords
- Galactic Center, disk warping, young massive stars, Wolf-Rayet stars, O-type stars, Sgr A*, stellar orbits, orbital plane orientation, angular momentum, in situ star formation, stellar streams, proper motions
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