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Hees A, Do T, Ghez AM, Martinez GD, Naoz S, Becklin EE, Boehle A, Chappell S, Chu D, Dehghanfar A, Kosmo K, Lu JR, Matthews K, Morris MR, Sakai S, Schödel R, Witzel G. Testing General Relativity with Stellar Orbits around the Supermassive Black Hole in Our Galactic Center. Phys Rev Lett 2017; 118:211101. [PMID: 28598651 DOI: 10.1103/physrevlett.118.211101] [Citation(s) in RCA: 15] [Impact Index Per Article: 2.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/22/2016] [Indexed: 06/07/2023]
Abstract
We demonstrate that short-period stars orbiting around the supermassive black hole in our Galactic center can successfully be used to probe the gravitational theory in a strong regime. We use 19 years of observations of the two best measured short-period stars orbiting our Galactic center to constrain a hypothetical fifth force that arises in various scenarios motivated by the development of a unification theory or in some models of dark matter and dark energy. No deviation from general relativity is reported and the fifth force strength is restricted to an upper 95% confidence limit of |α|<0.016 at a length scale of λ=150 astronomical units. We also derive a 95% confidence upper limit on a linear drift of the argument of periastron of the short-period star S0-2 of |ω[over ˙]_{S0-2}|<1.6×10^{-3} rad/yr, which can be used to constrain various gravitational and astrophysical theories. This analysis provides the first fully self-consistent test of the gravitational theory using orbital dynamic in a strong gravitational regime, that of a supermassive black hole. A sensitivity analysis for future measurements is also presented.
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Affiliation(s)
- A Hees
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
| | - T Do
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
| | - A M Ghez
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
| | - G D Martinez
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
| | - S Naoz
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
| | - E E Becklin
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
| | - A Boehle
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
| | - S Chappell
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
| | - D Chu
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
| | - A Dehghanfar
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
| | - K Kosmo
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
| | - J R Lu
- Astronomy Department, University of California, Berkeley, California 94720, USA
| | - K Matthews
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, MC 301-17, Pasadena, California 91125, USA
| | - M R Morris
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
| | - S Sakai
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
| | - R Schödel
- Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía S/N, 18008 Granada, Spain
| | - G Witzel
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
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Ackermann M, Ajello M, Albert A, Atwood WB, Baldini L, Ballet J, Barbiellini G, Bastieri D, Bechtol K, Bellazzini R, Berenji B, Blandford RD, Bloom ED, Bonamente E, Borgland AW, Bregeon J, Brigida M, Bruel P, Buehler R, Burnett TH, Buson S, Caliandro GA, Cameron RA, Cañadas B, Caraveo PA, Casandjian JM, Cecchi C, Charles E, Chekhtman A, Chiang J, Ciprini S, Claus R, Cohen-Tanugi J, Conrad J, Cutini S, de Angelis A, de Palma F, Dermer CD, Digel SW, do Couto e Silva E, Drell PS, Drlica-Wagner A, Falletti L, Favuzzi C, Fegan SJ, Ferrara EC, Fukazawa Y, Funk S, Fusco P, Gargano F, Gasparrini D, Gehrels N, Germani S, Giglietto N, Giordano F, Giroletti M, Glanzman T, Godfrey G, Grenier IA, Guiriec S, Gustafsson M, Hadasch D, Hayashida M, Hays E, Hughes RE, Jeltema TE, Jóhannesson G, Johnson RP, Johnson AS, Kamae T, Katagiri H, Kataoka J, Knödlseder J, Kuss M, Lande J, Latronico L, Lionetto AM, Llena Garde M, Longo F, Loparco F, Lott B, Lovellette MN, Lubrano P, Madejski GM, Mazziotta MN, McEnery JE, Mehault J, Michelson PF, Mitthumsiri W, Mizuno T, Monte C, Monzani ME, Morselli A, Moskalenko IV, Murgia S, Naumann-Godo M, Norris JP, Nuss E, Ohsugi T, Okumura A, Omodei N, Orlando E, Ormes JF, Ozaki M, Paneque D, Parent D, Pesce-Rollins M, Pierbattista M, Piron F, Pivato G, Porter TA, Profumo S, Rainò S, Razzano M, Reimer A, Reimer O, Ritz S, Roth M, Sadrozinski HFW, Sbarra C, Scargle JD, Schalk TL, Sgrò C, Siskind EJ, Spandre G, Spinelli P, Strigari L, Suson DJ, Tajima H, Takahashi H, Tanaka T, Thayer JG, Thayer JB, Thompson DJ, Tibaldo L, Tinivella M, Torres DF, Troja E, Uchiyama Y, Vandenbroucke J, Vasileiou V, Vianello G, Vitale V, Waite AP, Wang P, Winer BL, Wood KS, Wood M, Yang Z, Zimmer S, Kaplinghat M, Martinez GD. Constraining dark matter models from a combined analysis of Milky Way satellites with the Fermi Large Area Telescope. Phys Rev Lett 2011; 107:241302. [PMID: 22242987 DOI: 10.1103/physrevlett.107.241302] [Citation(s) in RCA: 34] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/18/2011] [Revised: 10/06/2011] [Indexed: 05/31/2023]
Abstract
Satellite galaxies of the Milky Way are among the most promising targets for dark matter searches in gamma rays. We present a search for dark matter consisting of weakly interacting massive particles, applying a joint likelihood analysis to 10 satellite galaxies with 24 months of data of the Fermi Large Area Telescope. No dark matter signal is detected. Including the uncertainty in the dark matter distribution, robust upper limits are placed on dark matter annihilation cross sections. The 95% confidence level upper limits range from about 10(-26) cm3 s(-1) at 5 GeV to about 5×10(-23) cm3 s(-1) at 1 TeV, depending on the dark matter annihilation final state. For the first time, using gamma rays, we are able to rule out models with the most generic cross section (∼3×10(-26) cm3 s(-1) for a purely s-wave cross section), without assuming additional boost factors.
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Affiliation(s)
- M Ackermann
- W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics, Stanford University, Stanford, California 94305, USA
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