Apoastron shift constraints on dark matter distribution at the Galactic Center

Zakharov, A. F.; Nucita, A. A.; Paolis, F. De; Ingrosso, G.

doi:10.1103/physrevd.76.062001

Cited by 77 publications

(69 citation statements)

References 34 publications

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“…Their analysis differs only slightly from that presented here in that it forces the focus to be at the inferred radio position of Sgr A Ã , assumes a Plummer model mass distribution, and is based on data presented in Eisenhauer et al (2003). Similarly, Zakharov et al (2007) use an order of magnitude analysis to show that if the total mass of the extended matter enclosed within the S0-2 orbit is k10 5 M , then it would produce a detectable apocenter shift Á k 10 mas (see also x 3.2 13 Allowing for the uncertainty in the LSR in V z (AE2 km s À1 ; Gould 2004) produces results that are not distinguishable from those reported for the V z ¼ 0 case. All contours are plotted at the 68%, 95%, and 99.7% confidence levels (equivalent to 1, 2, and 3 for a Gaussian distribution).…”

Section: Point Mass Plus Extended Mass Distribution Analysismentioning

confidence: 97%

Measuring Distance and Properties of the Milky Way’s Central Supermassive Black Hole with Stellar Orbits

Ghez

Salim

Weinberg

et al. 2008

Astrophysical Journal

1,512

1,601

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We report new precision measurements of the properties of our Galaxy's supermassive black hole. Based on astrometric (1995Y2007) and radial velocity (RV; 2000Y2007) measurements from the W. M. Keck 10 m telescopes, a fully unconstrained Keplerian orbit for the short-period star S0-2 provides values for the distance (R 0 ) of 8:0 AE 0:6 kpc, the enclosed mass (M bh ) of 4:1 AE 0:6 ; 10 6 M , and the black hole's RV, which is consistent with zero with 30 km s À1 uncertainty. If the black hole is assumed to be at rest with respect to the Galaxy (e.g., has no massive companion to induce motion), we can further constrain the fit, obtaining R 0 ¼ 8:4 AE 0:4 kpc and M bh ¼ 4:5 AE 0:4 ; 10 6 M . More complex models constrain the extended dark mass distribution to be less than 3Y4 ; 10 5 M within 0.01 pc, $100 times higher than predictions from stellar and stellar remnant models. For all models, we identify transient astrometric shifts from source confusion (up to 5 times the astrometric error) and the assumptions regarding the black hole's radial motion as previously unrecognized limitations on orbital accuracy and the usefulness of fainter stars. Future astrometric and RV observations will remedy these effects. Our estimates of R 0 and the Galaxy's local rotation speed, which it is derived from combining R 0 with the apparent proper motion of Sgr A Ã , ( 0 ¼ 229 AE 18 km s À1 ), are compatible with measurements made using other methods. The increased black hole mass found in this study, compared to that determined using projected mass estimators, implies a longer period for the innermost stable orbit, longer resonant relaxation timescales for stars in the vicinity of the black hole and a better agreement with the M bh -relation.

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Section: Point Mass Plus Extended Mass Distribution Analysismentioning

confidence: 97%

Measuring Distance and Properties of the Milky Way’s Central Supermassive Black Hole with Stellar Orbits

Ghez

Salim

Weinberg

et al. 2008

Astrophysical Journal

1,512

1,601

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“…We discuss and develop a method for studying the distribution of the dark matter at the center of the Galaxy by measuring the precession angle of orbits of S0 stars. For a number of particular cases, numerical calculations of the precession angle of orbits of S0 stars because of the extended mass distribution were performed [14][15][16][17][18][19]. We obtained general analytical formulas for the precession of orbits of stars with a powerlaw profile of the dark matter; these formulas make it possible to easily determine the additional distributed mass from the measured precession angle.…”

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confidence: 99%

Weighing of the dark matter at the center of the galaxy

Dokuchaev

Eroshenko

2015

Jetp Lett.

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A promising method for measuring the total mass of the dark matter near a supermassive black hole at the center of the Galaxy based on observations of nonrelativistic precession of the orbits of fast S0 stars together with constraints on the annihilation signal from the dark matter particles has been discussed. An analytical expression for the precession angle has been obtained under the assumption of a power-law profile of the dark matter density. In the near future, modern telescopes will be able to measure the precession of the orbits of S0 stars or to obtain a strong bound on it. The mass of the dark matter necessary for the explanation of the observed excess of gamma radiation owing to the annihilation of the dark matter particles has been calculated with allowance for the Sommerfeld effect.

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“…In 2008, astronomers finished observations for one orbital period of this star. At the beginning of these observations, astrometrical precision was at the level 10 mas, and since 2005 the astrometrical precision has been better than 1 mas, which practically coincides with the relativistic advance [85,86,87]. It is well-known that if there is a black hole alone (without a stellar cluster and a concentration of dark matter near a black hole) a test particle orbit is not elliptical, but there is so-called relativistic advance.…”

Section: 2018 1:42 Wspc/instruction File Zakharov˙icppa˙2017˙revimentioning

confidence: 99%

“…It is well-known that if there is a black hole alone (without a stellar cluster and a concentration of dark matter near a black hole) a test particle orbit is not elliptical, but there is so-called relativistic advance. In the case of a Kerr black hole, the relativistic advance depends on spin, but for the cases of S2 and S16, additional terms due to the presence of spin are roughly 100 times smaller than the classical value for the relativistic advance [85,86,87] (see also an updated discussion in [88,89]). …”

Section: 2018 1:42 Wspc/instruction File Zakharov˙icppa˙2017˙revimentioning

confidence: 99%

“…Therefore, in the future precise observations of bright stars will help to support, rule out or constrain some models of an extended mass distribution of stellar cluster and dark matter. For instance, in paper [86] we ruled out some theoretical models of dark matter distributions which were used earlier by astroparticle physicists to explain γ-ray flux from the Galactic Center with neutralino annihilation. Perhaps in the future, astronomers will get so stringent constraints on dark matter distribution that there will be no way to explain γ-flux from the Galactic Center region with neutralino annihilation [90].…”

Section: 2018 1:42 Wspc/instruction File Zakharov˙icppa˙2017˙revimentioning

confidence: 99%

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The black hole at the Galactic Center: Observations and models

Zakharov

2018

Int. J. Mod. Phys. D

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One of the most interesting astronomical objects is the Galactic Center. It is a subject of intensive astronomical observations in different spectral bands in recent years. We concentrate our discussion on a theoretical analysis of observational data of bright stars in the IR-band obtained with large telescopes. We also discuss the importance of VLBI observations of bright structures which could characterize the shadow at the Galactic Center. If we adopt general relativity (GR), there are a number of theoretical models for the Galactic Center, such as a cluster of neutron stars, boson stars, neutrino balls, etc. Some of these models were rejected or the range of their parameters is significantly constrained with consequent observations and theoretical analysis. In recent years, a number of alternative theories of gravity have been proposed because there are dark matter (DM) and dark energy (DE) problems. An alternative theory of gravity may be considered as one possible solution for such problems. Some of these theories have black hole solutions, while other theories have no such solutions. There are attempts to describe the Galactic Center with alternative theories of gravity and in this case one can constrain parameters of such theories with observational data for the Galactic Center. In particular, theories of massive gravity are intensively developing and theorists have overcome pathologies presented in the initial versions of these theories. In theories of massive gravity, a graviton is massive in contrast with GR where a graviton is massless. Now these theories are considered as an alternative to GR. For example, the LIGO–Virgo collaboration obtained the graviton mass constraint of about [Formula: see text] eV in their first publication about the discovery of the first gravitational wave detection event that resulted of the merger of two massive black holes. Surprisingly, one could obtain a consistent and comparable constraint of graviton mass at a level around [Formula: see text][Formula: see text]eV from the analysis of observational data on the trajectory of the star S2 near the Galactic Center. Therefore, observations of bright stars with existing and forthcoming telescopes such as the European extremely large telescope (E-ELT) and the thirty meter telescope (TMT) are extremely useful for investigating the structure of the Galactic Center in the framework of GR, but these observations also give a tool to confirm, rule out or constrain alternative theories of gravity. As we noted earlier, VLBI observations with current and forthcoming global networks (like the Event Horizon Telescope) are used to check the hypothesis about the presence of a supermassive black hole at the Galactic Center.

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Apoastron shift constraints on dark matter distribution at the Galactic Center

Cited by 77 publications

References 34 publications

Measuring Distance and Properties of the Milky Way’s Central Supermassive Black Hole with Stellar Orbits

Measuring Distance and Properties of the Milky Way’s Central Supermassive Black Hole with Stellar Orbits

Weighing of the dark matter at the center of the galaxy

The black hole at the Galactic Center: Observations and models

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