Issue 
A&A
Volume 615, July 2018



Article Number  L15  
Number of page(s)  10  
Section  Letters to the Editor  
DOI  https://doi.org/10.1051/00046361/201833718  
Published online  26 July 2018 
Letter to the Editor
Detection of the gravitational redshift in the orbit of the star S2 near the Galactic centre massive black hole^{⋆}
^{1}
Max Planck Institute for extraterrestrial Physics, Giessenbachstraße 1, 85748
Garching, Germany
^{2}
LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Univ. Paris Diderot, Sorbonne Paris Cité, 5 place Jules Janssen, 92195 Meudon, France
^{3}
Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
^{4}
1 st Institute of Physics, University of Cologne, Zülpicher Straße 77, 50937 Cologne, Germany
^{5}
Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
^{6}
Universidade de Lisboa – Faculdade de Ciências, Campo Grande, 1749016 Lisboa, Portugal
^{7}
Faculdade de Engenharia, Universidade do Porto, rua Dr. Roberto Frias, 4200465 Porto, Portugal
^{8}
European Southern Observatory, KarlSchwarzschildStraße 2, 85748 Garching, Germany
^{9}
European Southern Observatory, Casilla, 19001 Santiago 19, Chile
^{10}
Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Versoix, Switzerland
^{11}
Max Planck Institute for Radio Astronomy, Auf dem Hügel 69, 53121 Bonn, Germany
^{12}
Sterrewacht Leiden, Leiden University, Postbus 9513, 2300 RA Leiden, The Netherlands
^{13}
Departments of Physics and Astronomy, Le Conte Hall, University of California, Berkeley, CA, 94720 USA
^{14}
CENTRA – Centro de Astrofísica e Gravitação, IST, Universidade de Lisboa, 1049001 Lisboa, Portugal
^{15}
Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland
^{16}
European Space Agency, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
Received:
26
June
2018
Accepted:
29
June
2018
The highly elliptical, 16yearperiod orbit of the star S2 around the massive black hole candidate Sgr A^{✻} is a sensitive probe of the gravitational field in the Galactic centre. Near pericentre at 120 AU ≈ 1400 Schwarzschild radii, the star has an orbital speed of ≈7650 km s^{−1}, such that the firstorder effects of Special and General Relativity have now become detectable with current capabilities. Over the past 26 years, we have monitored the radial velocity and motion on the sky of S2, mainly with the SINFONI and NACO adaptive optics instruments on the ESO Very Large Telescope, and since 2016 and leading up to the pericentre approach in May 2018, with the fourtelescope interferometric beamcombiner instrument GRAVITY. From data up to and including pericentre, we robustly detect the combined gravitational redshift and relativistic transverse Doppler effect for S2 of z = Δλ / λ ≈ 200 km s^{−1}/c with different statistical analysis methods. When parameterising the postNewtonian contribution from these effects by a factor f , with f = 0 and f = 1 corresponding to the Newtonian and general relativistic limits, respectively, we find from posterior fitting with different weighting schemes f = 0.90 ± 0.09_{stat} ± 0.15_{sys}. The S2 data are inconsistent with pure Newtonian dynamics.
Key words: Galaxy: center / gravitation / black hole physics
This paper is dedicated to Tal Alexander, who passed away about a week before the pericentre approach of S2.
GRAVITY is developed in a collaboration by the Max Planck Institute for extraterrestrial Physics, LESIA of Paris Observatory/CNRS/Sorbonne Université/Univ. Paris Diderot and IPAG of Université Grenoble Alpes/CNRS, the Max Planck Institute for Astronomy, the University of Cologne, the CENTRA – Centro de Astrofisica e Gravitação, and the European Southern Observatory.
© ESO 2018
1. Introduction
General Relativity (GR) so far has passed all experimental tests with flying colours (Einstein 1916; Will 2014). The most stringent are tests that employ solar mass pulsars in binary systems (Kramer et al. 2006), and gravitational waves from 10 to 30 M_{⊙} black hole inspiral events (Abbott et al. 2016a,b,c). These tests cover a wide range of field strengths and include the strong curvature limit (Fig. A.2). At much lower field strength, Earth laboratories probe planetary masses that are about a factor 10^{6} lower than the stellar mass scale. For massive black hole (MBH) candidates with masses of 10^{6}−10 M_{⊙}, only indirect evidence for GR effects has been reported, such as relativistically broadened, redshifted iron Kα line emission in nearby active galaxies (Tanaka et al. 1995; Fabian et al. 2000). The closest MBH is at the centre of the Milky Way (R_{0} ≈ 8 kpc, M_{•} ≈ 4 × 10^{6}M_{⊙}), and its Schwarzschild radius subtends the largest angle on the sky of all known MBHs (R_{S} ≈ 10 µ as ≈ 0.08 AU). It is coincident with a very compact, variable Xray, infrared, and radio source, Sgr A^{✻}, which in turn is surrounded by a very dense cluster of orbiting young and old stars. Radio and infrared observations have provided detailed information on the distribution, kinematics, and physical properties of this nuclear star cluster and of the hot, warm, and cold interstellar gas interspersed in it (cf. Genzel et al. 2010; Morris et al. 2012; Falcke & Markoff 2013). Highresolution nearinfrared (NIR) speckle and adaptive optics (AO) assisted imaging and spectroscopy of the nuclear star cluster over the past 26 years, mainly by two groups in Europe (the Max Planck Institute for Extraterrestrial Physics, MPE, and the University of Cologne at the ESO New Technology Telecsope, NTT, and the Very Large Telescope, VLT) and one group in the USA (the University of California at Los Angeles, UCLA, at the Keck telescopes) have delivered more than 10^{4} stellar motions and orbit determinations for ≈45 individual stars (Schödel et al. 2002, 2009; Ghez et al. 2003, 2008; Eisenhauer et al. 2005; Gillessen et al. 2009b, 2017; Meyer et al. 2012; Boehle et al. 2016; Fritz et al. 2016). These orbits, in particular, the highly eccentric orbit of the mainsequence Bstar S2 (or S02 in the UCLA nomenclature), have demonstrated that the gravitational potential is dominated by a compact object of ≈4 × 10^{6}M_{⊙} that is concentrated within a pericentre distance from S2 of 17 light hours ≈14 mas or 120 AU from Sgr A^{✻}. S2 appears to be a single star (Martins et al. 2008; Habibi et al. 2017; GRAVITY Collaboration 2017; Chu et al. 2018), making it an ideal probe for testing GR by diffractionlimited imaging and spectroscopy (Alexander 2005; Zucker et al. 2006; Parsa et al. 2017), and interferometry (Grould et al. 2017) through the deviation of its apparent motion from a Keplerian orbit.
The radio source Sgr A^{✻} is coincident with the mass centroid to <1 mas (Plewa et al. 2015), and is itself very compact, with R (1.3 mm) < 18 µas ≈ 1.8 R _{S}, based on millimetre very long baseline interferometry (Falcke et al. 2000; Doeleman et al. 2008; Johnson et al. 2017). In addition, Sgr A^{✻} shows no detectable intrinsic motion, which supports the interpretation that the compact radio source is coincident with the mass (Reid & Brunthaler 2004; Reid 2009). The most conservative explanation for Sgr A^{✻} is that it is an MBH, assuming that GR is applicable (Genzel et al. 2010; Falcke & Markoff 2013; Vincent et al. 2016). So far, Newtonian orbits in a single central force potential can describe the motions of all stars. Any extended mass within the S2 orbit is lower than about 1% of the central mass (Hees et al. 2017; Gillessen et al. 2017).
2. Observations
We present^{1} an analysis of the positions and Kband spectra of the star S2 from 1992 to 2018 (Figs. 1 and 2).
Fig. 1.
Monitoring the S2 orbit around Sgr A^{✻} with the three VLT(I) instruments NACO (AOassisted, single UT imaging), GRAVITY (interferometric astrometryimaging with all four UTs of the VLT) and SINFONI (AOassisted integral field spectroscopy). Upper left: Deconvolved NACO Kband image of the Galactic centre a few weeks before the 2018 pericentre passage. The source S2 appears slightly elongated because of confusion with Sgr A^{✻}. Upper right: Nearly simultaneous GRAVITY image of S2 and Sgr A^{✻}. The image shows the central 150 mas (0.0059 pc ≈ 1.4 × 10^{4}R_{S}) after selfcalibration and CLEANing with AIPS. The image is reconstructed from 34 integrations of 5 min each from several nights at the end of March 2018. Sgr A^{✻} was (on average) K = 16.6 mag and the rms noise level of the background after cleaning is ≈20 mag. Both Sgr A^{✻} and S2 are unresolved. Here and in the other GRAVITY images, the elongation is due to the shape of the interferometric clean beam. Bottom: S2 – Sgr A^{✻} GRAVITY images (coaddition of several days) from July 2017 (bottom left) and May / June 2018, a few days after pericentre (bottom right). The inset in the bottom left panel shows the instantaneous interferometric beam, which is 2.2 mas × 4.7 mas without Earth rotation. The inset in the middle left shows a coadded SINFONI Kband spectrum of the star S2, taken from Habibi et al. (2017). 
Fig. 2.
Summary of the observational results of monitoring the S2 – Sgr A^{✻} orbit from 1992 to 2018. Left: projected orbit of the star S2 on the sky (J2000) relative to the position of the compact radio source Sgr A^{✻} (brown crossed square at the origin). Triangles and circles (and 1σ uncertainties) denote the position measurements with SHARP at the NTT and NACO at the VLT, colourcoded for time (colour bar on the right side). All data points are corrected for the bestfit zeropoint (x_{0}; y_{0}) and drifts (ẋ_{0}, ẏ_{0}) of the coordinate system relative to Sgr A^{✻} (see Plewa et al. 2015). Green squares mark the GRAVITY measurements. The bottom right panel shows a zoom around pericentre in 2018. Top right: radial velocity of S2 as a function of time (squares: SINFONI/NACO at the VLT; triangles: NIRC2 at Keck). S2 reached pericentre of its orbit at the end of April 2002, and then again on May 19th, 2018 (MJD 58257.67). The data before 2017 are taken from Ghez et al. (2008), Boehle et al. (2016), Chu et al. (2018), and Gillessen et al. (2017, 2009b). The 2017/2018 NACO/SINFONI and GRAVITY data are presented here for the first time. The cyan curve shows the bestfitting S2 orbit to all these data, including the effects of General and Special Relativity. 
We obtained skyprojected positions of the star S2 with the speckle camera SHARP at the NTT (1992–2002: Hofmann et al. 1993), but most of our imaging comes from the AOassisted NIR imager NACO at the VLT (2002–2018: Lenzen et al. 1998; Rousset et al. 1998) and the interferometric astrometryimager GRAVITY with all four Unit Telescopes (UTs) of the VLT interferometer (GRAVITY Collaboration 2017). The SHARP/NACO data deliver relative positions between stars in the nuclear star cluster. These are then registered with ≤ 1 mas precision in the radio frame of the Galactic centre (Reid et al. 2007) using multiepoch observations of nine SiO maser stars common between our infrared data and the radio interferometry, after correcting NACO image distortions with observations of a globular cluster calibrated on data from the Hubble Space Telescope (Plewa et al. 2015). In the GRAVITY interferometric observations, we detected and stabilised the interferometric fringes on the stars IRS16C or IRS16NW located ≈1″ from Sgr A^{✻}, and observed the “binary” S2 – Sgr A^{✻} within the second phasereferenced fibre (see GRAVITY Collaboration 2017). S2 and Sgr A^{✻} are simultaneously detected as two unresolved sources in > 90% of our individual integrations (5 min each), such that the S2 – Sgr A^{✻} vector is directly obtained in each of these measurements.
Our 2003–2018 measurements of the Brackettlineγ velocity were taken with the AOassisted integral field spectrometer SINFONI at the VLT (Eisenhauer et al. 2003a; Bonnet et al. 2004), with five additional 2000–2003 slitspectra from the AO imagers and spectrometers NIRC2 at Keck (see Ghez et al. 2003; Chu et al. 2018) and NACO (Eisenhauer et al. 2003b).
The 1992–2016 speckle and AOimaging and spectroscopic data used below have been presented in Gillessen et al. (2017). In 2017 and 2018 we increased the cadence of the observations in preparation for the pericentre approach in May 2018. We added 21 epochs of NACO K and Hband imaging in the 13 mas pix^{−1} scale, and 2 epochs of NACO Kband imaging in the 27 mas pix^{−1} scale to measure the SiO maser positions (Reid et al. 2007) that define our coordinate system (Plewa et al. 2015). We obtained 30 data sets of GRAVITY interferometry and 26 additional spectroscopy epochs with SINFONI using the 25 mas pix^{−1} scale and the combined H + Kband grating with a spectral resolution of R ≈ 1500.
For more details on the data analysis of all three instruments, we refer to Appendix A.
3. Results
3.1. Relativistic corrections
The left panel of Fig. 2 shows the combined singletelescope and interferometric astrometry of the 1992–2018 skyprojected orbital motion of S2, where the zero point is the position of the central mass and of Sgr A^{✻}. All NACO points were corrected for a zeropoint offset and drift in RA/Dec, which are obtained from the orbit fit. The bottom right panel zooms into the 2018 section of the orbit around pericentre measured with GRAVITY. The zoom demonstrates the hundredfold improvement of astrometry between SHARP in the 1990s (≈4 mas precision) and NACO in the 2000s (≈0:5 mas) to GRAVITY in 2018 (as small as ≈30 µas). While the motion on the sky of S2 could be detected with NACO over a month, the GRAVITY observations detect the motion of the star from day to day. The upper right panel of Fig. 2 displays the radial velocity measurements with SINFONI at the VLT and NIRC2 at Keck in the 1992–2018 period.
At pericentre R_{peri}, S2 moves with a total space velocity of ≈7650 km s^{−1}, or β = v/c = 2.55 × 10^{−2}. This means that the firstorder parameterised postNewtonian correction terms (PPN(1)), due to Special and General Relativity, beyond the orbital Doppler and Rømer effects, are within reach of current measurement precision, PPN(1) ~β^{2} ~ (R_{S}/R_{peri}) ~ 6.5 × 10^{−4}. These terms can be parameterised spectroscopically as (e.g. Misner et al. 1973; Alexander 2005; Zucker et al. 2006).
where the PPN(1)_{z} term B_{1} = B_{1,tD} + B_{1,gr}, with B_{1,tD} = B_{1,gr} = 0.5, and β^{2} = [R_{S}(1 + e)]/[2a(1 − e)] = 6:51 × 10^{−4} for S2. Here a is the semimajor axis and e is the eccentricity of the S2 orbit. B_{0.5}β is the Newtonian Doppler shift.
Equation (1) indicates that PPN(1)z consists in equal terms of the special relativistic transverse Doppler effect (B_{1,tD}) and the general relativistic gravitational redshift (B_{1,gr}), totalling ≈200 km s^{−1} redshift at pericentre, while at apocentre, it amounts to only 6 km s^{−}1. If the total orbital redshift z_{tot} is separated into a Newtonian/Kepler part z_{K} and a GR correction, one can write z_{tot} = z_{K} + f (z_{GR} − z_{K}), where f is zero for purely Newtonian physics and unity for GR. In the following we show the residuals Δz = z_{GR} − z_{K}. The Keplerian part of the orbit is at Δz = 0, and the PPN(1)_{z} corrections appear as an excess.
3.2. Analysis with prior Kepler orbit
We define a prior orbit K_{prior} by excluding those data for which the PPN(1)_{z} corrections matter. For K_{prior} we use the entire 1992–2018 SHARP/NACO and GRAVITY data and the SINFONI data from 2004 up to the end of 2016. We then obtained K_{prior} as described in Gillessen et al. (2017), which requires a simultaneous fit of 13 parameters. The Rømer delay is included in the calculation. The resulting orbit is a modest update of Gillessen et al. (2017). Using this as the prior orbit, we then added the radial velocities from 2017 and 2018 (Fig. 3). The 26 residual 2017/2018 spectroscopic data relative to Kprior clearly do not follow the bestfitting Keplerian orbit derived from all previous 51 spectroscopic and 196 positions in the past 26 years (grey line in Fig. 3), but instead follow the f = 1 (i.e. GR(K_{prior})) version of K_{prior} (red line in Fig. 3). This test is fair: GRcorrections should only be detectable with our measurement errors within ±1 year of pericentre.
Fig. 3.
Residual velocity c z = c(z_{GR} − z_{K}) for the best fitting prior Keplerian K_{prior} (f = 0, grey) and the same orbit with f = 1 (red GR_{prior}). K_{prior} was constructed from all 1992–2018 astrometric data with NACO & GRAVITY and the SINFONI data between 2004 and 2016 (open black circles). The 2017/2018 SINFONI data points (black circles with cyan shading) can then be added to test if the spectroscopic data around pericentre follow Kprior or the GR_{prior} predicted from K_{prior}. The new data points near and up to pericentre, where the β^{2} effects in radial velocity are expected to be important, fall close to the predicted GRprior curve, and exclude the Keplerian prior orbit. 
This a priori test demonstrates that the spectroscopic data around the pericenter passage are inconsistent with Newtonian dynamics and consistent with GR. However, both K_{prior} () and GR(K_{prior}) () are poor fits to the data.
3.3. Posterior analysis
Because of the uncertainties in the parameters of K_{prior}, in particular, in the strongly correlated mass and distance, a more conservative approach is to determine the bestfit value of the parameter f a posteriori, including all data and fitting for the optimum values of all parameters. In carrying out the fitting, it is essential to realise that the inferred measurement uncertainties are dominated by systematic effects, especially when evidence from three or more very different measurement techniques is combined (see Appendix A.6 for a more detailed discussion). In particular the NACO measurements are subject to correlated systematic errors, for example from unrecognised confusion events (Plewa & Sari 2018), which typically last for one year and are comparable in size to the statistical errors. We therefore downsampled the NACO data into 100 bins with equal path lengths along the projected orbit (Fig. 4, middle) and gave these data in addition a lower weight of 0.5. Depending on exactly which weighting or averaging scheme was chosen, the posterior analysis including all data between 1992 and 2018 yielded f values between 0.85 and 1.09. With a weighting of 0.5 of the NACO data, we find f = 0.90 ± 0.09 (Fig. 4). GR (f = 1) is favoured over pure Newtonian physics (f = 0) at the ≈10 σ level.
Fig. 4.
Posterior analysis of all data by fitting for f simultaneously with all other parameters. We plot the residuals in spectroscopy (top, NIRC2, NACO, and SINFONI), Dec and RA (middle two panels, filled grey: NACO; open grey: SHARP; green filled blue: GRAVITY) between the best f = 1 fit and the f = 0 (Newtonian) part of that fit for the model (red line) and all data. The black curve includes the Schwarzschild precession. Here, we downsampled the NACO data into 100 equal bins along the orbit to obtain a constant weighting in spatial coverage. With a weight of 0.5 for the NACO data (in order to account for the systematic errors), this yields a 10 σ result in favour of GR (f = 0.90 ± 0.09), and . The bottom panel shows the posterior probability distributions for f and its correlation with the mass M_{•} and distance R_{0} of the massive black hole, and the argument of periapsis ω. The distributions are compact and all parameters are well determined. 
The error on f is derived from the posterior probability distributions (Fig. 4, bottom) of a Markov chain Monte Carlo (MCMC) analysis. Fig. A.1 shows the full set of correlation plots and probability distributions for the fit parameters. The distributions are compact and all parameters are well determined. The bestfit values and uncertainties are given Table A.1.
The superb GRAVITY astrometry demonstrably improves the quality of the fits and is crucial for overcoming the source confusion between Sgr A^{✻} and S2 near pericentre. A minimal detection of PPN(1)_{z} (Eq. (1)) is provided by a combination using only NACO and SINFONI data (f_{NACO + SINFONI} = 0.71 ± 0.19, 3.6 σ), but the inclusion of the GRAVITY data very significantly improves the precision and significance of the fitted parameters: the improvement reaches a factor of 2–3.
A still more demanding test is to search for any Keplerian fit to all data and determine whether its goodness of fit is significantly poorer than the goodness of fit of the bestfitting GRorbit. For linear models the formula presented in Andrae et al. (2010) can be used to estimate the significance. However, the value for the degrees of freedom (d.o.f.) is not well defined for nonlinear models (Andrae et al. 2010). In our case, we have two models that only differ significantly over a very critical short timespan given the uncertainties in the underlying data. We therefore used the number of those data points as d.o.f. for which the two models predict significant differences. The difference in χ^{2} yields a formal significance of 5 σ or greater in favour of the relativistic model.
For further comments on a Bayesian analysis of our data, see Appendix A.9.
4. Discussion
We have reported the first direct detection of the PPN(1) gravitational redshift parameter around the MBH in the Galactic centre from a data set that extends up to and includes the pericentre approach in May 2018. Three different analysis methods of our data suggest that this detection favours the postNewtonian model with robust significance. Further improvement of our results is expected as our monitoring continues post pericentre. Still, there are reasons to be cautious about the significance of these early results, mainly because of the systematic effects and the validity of our basic assumptions and model. The most important concern probably is that our basic input model (a binary consisting of an MBH and a star with much lower mass) is incomplete. Additional “luminous” and massive objects around S2 and between S2 and Sgr A^{✻} are unlikely given the spectroscopic and imaging data. Based on the radial velocities of S2, Chu et al. (2018) excluded any companion with Msin(i) < 1.6 M_{⊙} for periods up to 150 days, the longest period for which the binary is not subject to tidal breakup. The GRAVITY imaging data (Fig. 1) so far do not show any object near Sgr A^{✻} and S2 brighter than K ≈ 18.5 mag, corresponding to a 2 M_{⊙} mainsequence star. However, massive, nonluminous objects, such as stellar black holes, might be present and could affect the orbital dynamics of S2 (Gualandris & Merritt 2009; Merritt et al. 2010; Gualandris et al. 2010). We repeated the exercise by Gillessen et al. (2017) of testing how much of an extended mass distribution (in form of a Plummer distribution) could still be commensurable with our full new data set. We find that such an extended mass is lower than 0.35– 1% of the central mass, depending on the assumed Plummer radius.
The next relativistic correction term we hope to detect is the Schwarzschild precession, which per orbital revolution is(2)
Since the precession is strongly dependent on distance from the black hole and S2 is on a highly elliptical orbit, the term manifests itself as a kink between the incoming nearKeplerian and the outgoing nearKeplerian orbit. In addition, it leads to a westward drift of all data points around apocentre. The posterior fit of the current data including the Schwarzschild precession yields an f value still closer to GR than without the precession term (f = 0.94 ± 0.09). The chances for robustly detecting the Schwarzschild precession with further observations are very high. GRAVITY will continue to be critical for this second phase of the experiment. Our forecast suggests that we will obtain a 5 σ posteriori result with GRAVITY by 2020 (Grould et al. 2017).
Acknowledgments
We are very grateful to our funding agencies (MPG, ERC, CNRS, DFG, BMBF, Paris Observatory, Observatoire des Sciences de l’Univers de Grenoble, and the Fundação para a Ciência e Tecnologia), to ESO and the ESO/Paranal staff, and to the many scientific and technical staff members in our institutions who helped to make NACO, SINFONI, and GRAVITY a reality. S.G., P.P., C.D., N.B., and Y.K. acknowledge support from ERC starting grant No. 306311. F.E. and O.P. acknowledge support from ERC synergy grant No. 610058. We also would like to acknowledge the important theoretical contributions of the late Tal Alexander (Weizmann Institute, Rehovot), whose 2006 paper with Shay Zucker and members of the MPE group encouraged us to pursue this project. Unfortunately, Tal missed seeing the fruits of this effort by only a few weeks.
Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 075.B0547, 076.B0259, 077.B0014, 078.B0136, 179.B0261, 183.B0100, 087.B0117, 088.B0308, 288.B5040, 089.B0162, 091.B0081, 091.B0086, 091.B0088, 092.B0238, 092.B0398, 093.B0217, 093.B0218, 594.B0498, 097.B0050, 598.B0043, 299.B5014, 299.B5056, 099.B0162, 0100.B0731, 0101.B0195, and 0101.B0576.
References
 Abbott, B. P., Abbott, R., Abbott, T. D., et al. 2016a, ApJ, 818, L22 [Google Scholar]
 Abbott, B. P., Abbott, R., Abbott, T. D., et al. 2016b, Phys. Rev. Lett., 116, 241103 [Google Scholar]
 Abbott, B. P., Abbott, R., Abbott, T. D., et al. 2016c, Phys. Rev. Lett., 116, 061102 [Google Scholar]
 Alexander, T. 2005, Phys. Rep., 419, 65 [NASA ADS] [CrossRef] [Google Scholar]
 Andrae, R., SchulzeHartung, T., & Melchior, P. 2010, ArXiv eprints [arXiv: 1012.3754] [Google Scholar]
 Anugu, N., Amorim, A., Gordo, P., et al. 2018, MNRAS, 476, 459 [NASA ADS] [CrossRef] [Google Scholar]
 Bardeen, J. M., & Petterson, J. A. 1975, ApJ, 195, L65 [NASA ADS] [CrossRef] [Google Scholar]
 Baron, F., Monnier, J. D., & Kloppenborg, B. 2010, in Optical and Infrared Interferometry II, Proc. SPIE, 7734, 77342I [Google Scholar]
 Barstow, M. A., Bond, H. E., Holberg, J. B., et al. 2005, MNRAS, 362, 1134 [CrossRef] [Google Scholar]
 Boehle, A., Ghez, A. M., Schödel, R., et al. 2016, ApJ, 830, 17 [NASA ADS] [CrossRef] [Google Scholar]
 Bonnet, H., Abuter, R., Baker, A., et al. 2004, The Messenger, 117, 17 [NASA ADS] [Google Scholar]
 Chu, D. S., Do, T., Hees, A., et al. 2018, ApJ, 854, 12 [Google Scholar]
 Doeleman, S. S., Weintroub, J., Rogers, A. E. E., et al. 2008, Nature, 455, 78 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Einstein, A. 1916, Ann. Phys., 354, 769 [Google Scholar]
 Eisenhauer, F., Abuter, R., Bickert, K., et al. 2003a, in Instrument Design and Performance for Optical/Infrared Groundbased Telescopes, eds. M. Iye, & A. F. M. Moorwood, Proc. SPIE, 4841, 1548 [Google Scholar]
 Eisenhauer, F., Schödel, R., Genzel, R., et al. 2003b, ApJ, 597, L121 [NASA ADS] [CrossRef] [Google Scholar]
 Eisenhauer, F., Genzel, R., Alexander, T., et al. 2005, ApJ, 628, 246 [NASA ADS] [CrossRef] [Google Scholar]
 Fabian, A. C., Iwasawa, K., Reynolds, C. S., & Young, A. J. 2000, PASP, 112, 1145 [NASA ADS] [CrossRef] [Google Scholar]
 Falcke, H., & Markoff, S. B. 2013, Class. Quant. Grav., 30, 244003 [Google Scholar]
 Falcke, H., Melia, F., & Agol, E. 2000, ApJ, 528, L13 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Fritz, T. K., Chatzopoulos, S., Gerhard, O., et al. 2016, ApJ, 821, 44 [NASA ADS] [CrossRef] [Google Scholar]
 GallegoCano, E., Schödel, R., Dong, H., et al. 2018, A&A, 609, A26 [Google Scholar]
 Genzel, R., Schödel, R., Ott, T., et al. 2003, ApJ, 594, 812 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Genzel, R., Eisenhauer, F., & Gillessen, S. 2010, Rev. Mod. Phys., 82, 3121 [NASA ADS] [CrossRef] [Google Scholar]
 Ghez, A. M., Duchêne, G., Matthews, K., et al. 2003, ApJ, 586, L127 [NASA ADS] [CrossRef] [Google Scholar]
 Ghez, A. M., Salim, S., Weinberg, N. N., et al. 2008, ApJ, 689, 1044 [NASA ADS] [CrossRef] [Google Scholar]
 Gillessen, S., Eisenhauer, F., Fritz, T. K., et al. 2009a, ApJ, 707, L114 [NASA ADS] [CrossRef] [Google Scholar]
 Gillessen, S., Eisenhauer, F., Trippe, S., et al. 2009b, ApJ, 692, 1075 [NASA ADS] [CrossRef] [Google Scholar]
 Gillessen, S., Plewa, P. M., Eisenhauer, F., et al. 2017, ApJ, 837, 30 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 GRAVITY Collaboration (Abuter, R., et al.) 2017, A&A, 602, A94 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Greenstein, J. L., Oke, J. B., & Shipman, H. L. 1971, ApJ, 169, 563 [NASA ADS] [CrossRef] [Google Scholar]
 Greisen, E. W. 2003, in Information Handling in Astronomy – Historical Vistas, ed. A. Heck, Astrophysics and Space Science Library, 285, 109 [NASA ADS] [CrossRef] [Google Scholar]
 Grould, M., Vincent, F. H., Paumard, T., & Perrin, G. 2017, A&A, 608, A60 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Gualandris, A., Gillessen, S., & Merritt, D. 2010, MNRAS, 409, 1146 [NASA ADS] [CrossRef] [Google Scholar]
 Gualandris, A., & Merritt, D. 2009, ApJ, 705, 361 [NASA ADS] [CrossRef] [Google Scholar]
 Habibi, M., Gillessen, S., Martins, F., et al. 2017, ApJ, 847, 120 [NASA ADS] [CrossRef] [Google Scholar]
 Hees, A., Do, T., Ghez, A. M., et al. 2017, Phys. Rev. Lett., 118, 211101 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Hofmann, R., Eckart, A., Genzel, R., & Drapatz, S. 1993, Ap&SS, 205, 1 [NASA ADS] [CrossRef] [Google Scholar]
 Högbom, J. A. 1974, A&AS, 15, 417 [Google Scholar]
 Johnson, M. D., Bouman, K. L., Blackburn, L., et al. 2017, ApJ, 850, 172 [NASA ADS] [CrossRef] [Google Scholar]
 Kramer, M., Stairs, I. H., Manchester, R. N., et al. 2006, Science, 314, 97 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Lachaume, R., & Berger, J.P. 2013, MNRAS, 435, 2501 [NASA ADS] [CrossRef] [Google Scholar]
 Lapeyrere, V., Kervella, P., Lacour, S., et al. 2014, in Optical and Infrared Interferometry IV, Proc. SPIE, 9146, 91462D [Google Scholar]
 Lenzen, R., Hofmann, R., Bizenberger, P., & Tusche, A. 1998, in Infrared Astronomical Instrumentation, ed. A. M. Fowler, Proc. SPIE, 3354, 606 [NASA ADS] [CrossRef] [Google Scholar]
 Mackay, D. J. C. 2003, Information Theory, Inference and Learning Algorithms, 640 [Google Scholar]
 Martins, F., Gillessen, S., Eisenhauer, F., et al. 2008, ApJ, 672, L119 [NASA ADS] [CrossRef] [Google Scholar]
 Merritt, D., Alexander, T., Mikkola, S., & Will, C. M. 2010, Phys. Rev. D, 81, 062002 [NASA ADS] [CrossRef] [Google Scholar]
 Meyer, L., Ghez, A. M., Schödel, R., et al. 2012, Science, 338, 84 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Misner, C. W., Thorne, K. S., & Wheeler, J. A. 1973, Gravitation [Google Scholar]
 Morris, M. R., Meyer, L., & Ghez, A. M. 2012, Res. Astron. Astrophys., 12, 995 [NASA ADS] [CrossRef] [Google Scholar]
 Parsa, M., Eckart, A., Shahzamanian, B., et al. 2017, ApJ, 845, 22 [NASA ADS] [CrossRef] [Google Scholar]
 Plewa, P. M., Gillessen, S., Eisenhauer, F., et al. 2015, MNRAS, 453, 3234 [NASA ADS] [CrossRef] [Google Scholar]
 Plewa, P. M., & Sari, R. 2018, MNRAS, 476, 4372 [NASA ADS] [CrossRef] [Google Scholar]
 Pound, R. V., & Rebka, G. A. 1959, Phys. Rev. Lett., 3, 439 [NASA ADS] [CrossRef] [Google Scholar]
 Psaltis, D. 2004, in Xray Timing 2003: Rossi and Beyond, eds. P. Kaaret, F. K. Lamb, & J. H. Swank, American Institute of Physics Conference Series, 714, 29 [Google Scholar]
 Reid, M. J. 2009, Int. J. Mod. Phys. D, 18, 889 [NASA ADS] [CrossRef] [Google Scholar]
 Reid, M. J., & Brunthaler, A. 2004, ApJ, 616, 872 [NASA ADS] [CrossRef] [Google Scholar]
 Reid, M. J., Menten, K. M., Trippe, S., Ott, T., & Genzel, R. 2007, ApJ, 659, 378 [NASA ADS] [CrossRef] [Google Scholar]
 Rousset, G., Lacombe, F., Puget, P., et al. 1998, in Adaptive Optical System Technologies, eds. D. Bonaccini, & R. K. Tyson, Proc. SPIE, 3353, 508 [NASA ADS] [CrossRef] [Google Scholar]
 Sabha, N., Eckart, A., Merritt, D., et al. 2012, A&A, 545, A70 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Scheithauer, S., Brandner, W., Deen, C., et al. 2016, in Adaptive Optics Systems V, Proc. SPIE, 9909, 99092L [NASA ADS] [CrossRef] [Google Scholar]
 Schödel, R., Ott, T., Genzel, R., et al. 2002, Nature, 419, 694 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Schödel, R., Merritt, D., & Eckart, A. 2009, A&A, 502, 91 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Schödel, R., GallegoCano, E., Dong, H., et al. 2018, A&A, 609, A27 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Tanaka, Y., Nandra, K., Fabian, A. C., et al. 1995, Nature, 375, 659 [NASA ADS] [CrossRef] [Google Scholar]
 Tatulli, E., Millour, F., Chelli, A., et al. 2007, A&A, 464, 29 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Taylor, J. H., & Weisberg, J. M. 1982, ApJ, 253, 908 [NASA ADS] [CrossRef] [Google Scholar]
 Thiébaut, E. 2008, in Optical and Infrared Interferometry, Proc. SPIE, 7013, 70131I [Google Scholar]
 Vincent, F. H., Meliani, Z., Grandclément, P., Gourgoulhon, E., & Straub, O. 2016, Class. Quant. Grav., 33, 105015 [NASA ADS] [CrossRef] [Google Scholar]
 Waisberg, I., Dexter, J., Gillessen, S., et al. 2018, MNRAS, 476, 3600 [NASA ADS] [CrossRef] [Google Scholar]
 Will, C. M. 2008, ApJ, 674, L25 [Google Scholar]
 Will, C. M. 2014, Liv. Rev. Rel., 17, 4 [Google Scholar]
 Zucker, S., Alexander, T., Gillessen, S., Eisenhauer, F., & Genzel, R. 2006, ApJ, 639, L21 [NASA ADS] [CrossRef] [Google Scholar]
Appendix A: Supplementary material
A.1. NACO and SINFONI data analysis
The data reduction and analysis tools are almost identical to what we used in Gillessen et al. (2017), such that in the following section we concentrate on the specific aspects relevant for the excess redshift. We do not use the “combined” data set in the sense of Gillessen et al. (2009a), that is, we do not include the astrometric data set presented in Boehle et al. (2016), but use NTT and VLT astrometry only. This facilitates fitting because it removes four fit parameters.
In 2018, the NACO point spread functions (PSF) for S2 and Sgr A^{✻} overlap, such that confusion affects the S2 positions at the mas level, similar to the data in 2002 (Ghez et al. 2008; Gillessen et al. 2009b). Fortunately, the GRAVITY astrometry is not affected by this confusion problem and improves the 2017/2018 astrometry to a precision of 30−150 µas. In the case of NACO, fainter and sofar unknown stars might be present in the field and could result in 0.5−1 mas positional offsets from undetected source confusion throughout the S2 orbit, which typically lasts for about one year (Plewa & Sari 2018).
Another critical aspect is the precision of radial velocity measurements of S2. It is a K_{s} ≈ 14 mag star, for which the HI n = 7 − 4 recombination line (Brackettγ, λ = 2.1661 µm) and the HeI (λ = 2.112 µm) line can be detected in absorption at >5 σ per spectral resolution element in one hour. The wavelength calibration is finetuned in each individual exposure by comparing the positions of the atmospheric OHemissionlines with their expected positions. In the wavelength regime in which the S2 Brγ line is currently observed, we use approximately a dozen lines, and the scatter of the OHlines after the finetuning around the expected positions is below 5 km s^{−1}, which is smaller than the scatter in the Brγ data. We hence estimate that our systematic uncertainty due to the wavelength calibration is 5 km s^{−1}. The dominant error term, however, is the correction from residual sky features in the data. Given that S2 changes its radial velocity quickly and that these residuals vary from one observation to the next, we can assume that they essentially act as a random error. In practice, typical 1 σ uncertainties of the line centres are ±12 to ±20 km s^{−1}. At some observation epochs, confusion with other stars or extended nebular emission (mainly at low velocities) or atmospheric residuals leads to increased uncertainties. The line shape of S2 might be affected by a stellar wind, although previous analyses suggest that S2 is a mainsequence dwarf with low rotational velocity, which is not expected to have significant mass loss (Martins et al. 2008; Habibi et al. 2017). The stacked spectrum of S2 with a very high signaltonoise ratio of ≈200, newly obtained during the pericentre passage (March– June 2018), does not show a P Cygni profile either, which would be indicative of a wind. If a wind component were to introduce a constant bias, it would affect the accuracy, but not the precision by which we measure the redshift of S2. In the fit, this would in turn be absorbed into the motion of the reference system in the direction of the line of sight. If the shape of the spectrum is variable due to the wind, we would obtain a lower precision on the radial velocities. So far, no hints of a variable spectrum of S2 have been seen, and the classification of S2 as a B2.5 mainsequence star argues against spectral variability (Habibi et al. 2017). Moreover, we use a crosscorrelation with the observed S2 spectrum (Martins et al. 2008; Habibi et al. 2017) in addition to a line fit, which would most likely be affected in a different way than the single line. The two ways of determining the radial velocity agree very well, which demonstrates that the line shape of the Brγ line does not affect our measurement.
A.2. GRAVITY observations
The GRAVITY observations were taken at the Very Large Telescope Interferometer in Chile. The instrument coherently combines the light of the four 8m UTs. We chose the most sensitive low spectral resolution mode of GRAVITY (GRAVITY Collaboration 2017). In this mode, the science spectrum is dispersed across 14 pixels with a spectral resolving power of R ≈ 20. Nearly all data were taken in split polarisation mode, with a Wollaston prism inserted in the optical train and the two linear polarisations recorded independently.
All four UTs locked their Coudé infrared AO (CIAO, Scheithauer et al. 2016) module on the brightest source in the field, the red supergiant IRS7 (m_{K} ≈ 6.5 mag, distance from Sgr A^{✻} ≈ 5.5″). Active field and pupil guiding was enabled (Anugu et al. 2018). The interferometric observations started with IRS16NW or IRS16NE feeding the fringetracker and IRS16C feeding the science channel. These two bright stars (m_{K} ≈ 10.0–10.5 mag, separation from Sgr A^{✻} ≈1″) were used to find fringes and to zero the optical delay of the science channel. The actual observations of S2 and Sgr A^{✻} were then made with IRS16C or IRS16NW as fringetracking star. Each science exposure consists of 30 frames with an individual integration time of 10s each. The typical observing sequence had five such 5min exposures on Sgr A^{✻}, one exposure on S2, one sky exposure, and one exposure on R2, a moderately bright (m_{K} ≈ 12.1 mag, separation ≈1.5″) nearby unresolved giant star, which served as a visibility calibrator. This sequence was repeated several times per night.
A.3. GRAVITY data analysis
We used the standard GRAVITY pipeline to process the data (Lapeyrere et al. 2014; GRAVITY Collaboration 2017). Each individual exposure was first sky subtracted, flat fielded, and wavelength calibrated. The data were then reduced based on a pixeltovisibility matrix (P2VM, Tatulli et al. 2007), which represents the instrument transfer function including throughput, coherence, phase shift, and crosstalk information of each individual pixel. In a second step, the science complex visibilities are phasereferenced to the fringetracker complex visibilities using the laser metrology and a fiber dispersion model. The observatory transfer function (i.e. coherence loss due to vibrations, uncorrected atmosphere, birefringence, etc.) was calibrated on the nearby unresolved calibrator star R2.
A.4. Model fitting
The reported astrometric positions are based on a twocomponent binary fit to the (squared) visibilities and closure phases. We took into account the flux ratio between S2 and Sgr A^{✻}, the colour of Sgr A^{✻}, bandwidth smearing (e.g. Lachaume & Berger 2013), and a telescopedependent injection ratio. We developed several independent fitting codes, employing leastsquares minimization, MCMC optimization, and a combination of these two techniques. A full mathematical derivation of the models is beyond the scope of this paper. Overall, the results agree very well independent of the optimization technique and the detailed implementation.
A.5. Imaging
Complementary to the model fitting, we reconstructed images using radio and optical interferometry imaging tools. By employing different codes, we checked for consistency and robustness.
The radiointerferometrylike imaging was done with the Astronomical Imaging Process System (AIPS, Greisen 2003) developed at NRAO. For each exposure, we reconstructed the dirty image by a discrete Fourier transform of the complex visibility data. We then extracted preliminary images of S2 using the CLEAN algorithm (e.g. Högbom 1974) with clean boxes only on the brightest features of the dirty image. After this, we performed phasebased selfcalibration of the visibility data with the preliminary S2 model to correct for telescopebased errors. Then we reran CLEAN on the selfcalibrated data to clean both on S2 and Sgr A^{✻} iteratively, resulting in one image per exposure. In a last step, we combined individual exposures to obtain the final image for each night.
We also made use of MiRA2 (Thiébaut 2008) and Squeeze (Baron et al. 2010), two optical interferometry imaging codes. These codes fit an image to the data using a leastsquares minimization (MiRA2) or MCMC (Squeeze) with some penalty function to account for the sparsity of the data. The advantage of these codes is that they can account for coherence losses due to bandwidth smearing, and that they can also work directly with the robust closurephases, thereby avoiding the selfcalibration described above. Their weakness, however, is that the result depends on the chosen penalty function (priors), and fit convergence can be an issue.
A.6. Treatment of systematic uncertainties
As discussed above, all of the major observational input data in this paper (NACO, SINFONI, GRAVITY) are affected by strong and different systematic effects. NACO positional measurements are affected by obvious or unrecognized confusion events, especially close to Sgr A^{✻} (typically lasting one year, Plewa & Sari 2018) and have to be tied into a longterm reference frame coupled to the radio interferometric frame. Stars common to both frames but spread over tens of arcseconds are used for this alignment, but they in turn require a careful analysis of image distortions and mosaicking shifts (Plewa et al. 2015). As a result, the S2 positions can at times have systematic uncertainties exceeding 1 mas, although the statistical errors are ≈ 0.4−0.6 mas. Depending on the redshift, SINFONI spectroscopic data can be affected more or less strongly by atmospheric sky lines and extended nebular emission in the central cluster. This means that velocity uncertainties can exceed the typical performance in good conditions of 10−15 km s^{−1}. GRAVITY astrometry offers by far the best expected positional information (30−150 µas). However, the current accuracy is still limited by systematics and calibration errors, especially if Sgr A^{✻} is particularly faint, is varying during the integration, or if the S2 – Sgr A^{✻} separation is very large and close to the limit of the interferometric and photometric field of view, as was the case in 2017.
Our approach to account for these effects was to have several team members use different analysis tools for positional fitting and extraction, and to compare and average these results, with the analysis scatter providing an estimate of the systematic effects. Bootstrapping and removal of questionable data sets was performed in all cases. Every new observing epoch will add to the understanding of the systematic effects, and we expect to further improve especially the astrometric accuracy of GRAVITY in the coming years.
A.7. Rømer effect
Both gravitational redshift and transverse Doppler effect are of the order of β ^{2}. As Zucker et al. (2006) have pointed out, the classical Rømer delay also needs to be taken into account at that level. Including the light travel time requires solving the equation(A.1)
where x denotes the lineofsight distance, t_{em} the time of emission, and t_{obs} the time of observation. This equation can only be solved iteratively, which is done in some of our codes. However, one can also approximate the correction term by(A.2)
which can be evaluated without iteration, and is thus more suitable for a fitting algorithm. For the S2 orbit, the correction term varies by around eight days over the orbit, and the approximation never differs by more than 10 s from the exact solution. Some of our fitting codes therefore use the approximation to calculate the Rømer delay. Light bending (lensing and Shapiro time delay) effects on positions (≈20 µas) and velocities (≈5 km s^{−1}) can be neglected at the current precision.
A.8. Degeneracy between special relativistic effects and gravitational redhift
In Eq. (1), the special relativistic transverse Doppler effect and the gravitational redshift are completely degenerate. The degeneracy is broken only by the relative motion between observer and massive black hole, which is mostly due to the solar orbit in the Milky Way. The apparent motion of Sgr A^{✻} of about 240 km s^{−1} along the Galactic plane towards the southwest (Reid & Brunthaler 2004) leads to a correction term that is of the order of +5 km s^{−1} at pericentre and −0.2 km s^{−1} at apocentre. Earth’s motion around the Sun will contribute a term that is smaller by an order of magnitude. Overall, the effect of the relative motion between observer and Sgr A^{✻} is too small to break the degeneracy. We therefore use the standard local standard of rest (LSR) correction and accept the complete degeneracy.
A.9. MCMC analysis
As discussed in the main text, we carried out posteriori analyses of all data by fitting 14 parameters characterising the NACO reference frame relative to Sgr A^{✻} (x_{0}, y_{0}, ẋ_{0}, ẏ_{0}, ż_{0}), the central mass M_{•}, its distance from the Sun R_{0}, the Keplerian orbit parameters a, e, i, Ω ω, T_{peri}, and the parameter f introduced in section 3 to distinguish between Newtonian/Keplerian dynamics (f = 0) and the combined special and general relativistic effects up to PPN(1)_{z} (f = 1). Table A.1 lists the bestfit solution for the entire data set as treated in Fig. 4 (left without, and right with Schwarzschild precession) for a weight of 0.5 of the downsampled NACO data. Fig. A.1 gives the posterior parameter distributions of this fit.
Bestfit orbit parameters with and without Schwarzschild precession.
Fig. A.1.
Posterior probability distributions obtained from a Markov chain for the 14parameter fit including f as a free parameter. All parameters are well constrained, in particular also f . We have omitted the panels corresponding to the four coordinate system parameters in this figure for clarity. 
For the purpose of model comparison in a Bayesian framework, we use the fact that the posterior probability distribution is well described by a multivariate Gaussian in both cases (f = 0 and f = 1). We can thus use the respective peak (bestfit) parameter values and the covariance matrices to approximate the Bayesian evidence integrals (Mackay 2003). The ratio of the socalled Occam factors describing the ratio of the volumes of the two posterior parameter spaces is almost unity, such that the evidence ratio ρ equals the likelihood ratio, i.e. ρ ≈ Δχ^{2}/2, which is ≈ 43 in favour of f = 1 (assuming p(f = 0) = p(f = 1) a priori). The differences in the Bayesian information criteria (BIC) and the Akaike information criteria (AIC) both equal Δχ^{2} in our case. Given that Δχ^{2} = 87, we have a “decisive” evidence for f = 1 when applying Jeffrey’s scale.
We estimated the sampling error on f by means of a bootstrap analysis, during which we randomised the astrometric and spectroscopic data points separately but simultaneously. We refit the bootstrap sample and used the standard deviation of the bestfit values of f as sampling error. We obtain Δf = 0.15.
A.10. LenseThirring effect
The S2 experiment delivers a valuable confirmation of GR in a sofar unexplored regime at high masses (Fig. A.2, adapted from Psaltis 2004). A further goal would be determining the spin of the massive black hole through the combination of frame dragging and quadrupole moment, the socalled LenseThirring (LT) precession, of PPN(1.5) order (e.g. Misner et al. 1973; Bardeen & Petterson 1975; Will 2008):(A.3)
Fig. A.2.
Comparison of tests of General Relativity, inspired by Psaltis (2004). Shown in black are wellestablished tests: the Pound & Rebka (1959) experiment, the precession of Mercury (Einstein 1916), light deflection and the Shapiro delay in the solar system, the HulseTaylor pulsar (Taylor & Weisberg 1982), the gravitational redshift of Sirius B (Greenstein et al. 1971; Barstow et al. 2005), the LIGO detections (Abbott et al. 2016a,c,b), and the relativistic Fe Kα line (Tanaka et al. 1995; Fabian et al. 2000). Future tests are shown in grey, and this work, which uses the S2 orbit around Sgr A^{✻}, is shown in blue. 
where ξ ≤ 1 is the dimensionless spin parameter of a Kerr black hole. For ξ = 0.5, the LT precession of S2 is 9″, which is clearly not detectable. It is thus necessary to observe stars yet deeper in the potential if the spin of Sgr A^{✻} is to be measured with orbiting stars. Waisberg et al. (2018) have quantitatively analysed the requirements for detecting the LTprecession on a star inside the S2 orbit. They find that such a star would have to have a combination of semimajor axis a and eccentricity e, a(1 − e^{2})^{3/4}/R_{S} ≤ 250, and a significant detection would require 10 µas astrometric precision in a campaign over several years. Based on the Kband luminosity function (Genzel et al. 2003; Sabha et al. 2012; GallegoCano et al. 2018; Schödel et al. 2018) and the eccentricity distribution of the Sstars (Gillessen et al. 2017), Waisberg et al. (2018) estimate a probability of ≈10 % for a K < 19 mag star to fulfill the above requirement. Still fainter stars would likely be more common. No second star with K < 18.5 mag has so far been reliably detected near Sgr A^{✻} with GRAVITY, which is consistent with the predictions of Waisberg et al. (2018). We hope for such a detection in the next years, when S2 has moved away from Sgr A^{✻} and cleared the field of view for fainter objects.
All Tables
All Figures
Fig. 1.
Monitoring the S2 orbit around Sgr A^{✻} with the three VLT(I) instruments NACO (AOassisted, single UT imaging), GRAVITY (interferometric astrometryimaging with all four UTs of the VLT) and SINFONI (AOassisted integral field spectroscopy). Upper left: Deconvolved NACO Kband image of the Galactic centre a few weeks before the 2018 pericentre passage. The source S2 appears slightly elongated because of confusion with Sgr A^{✻}. Upper right: Nearly simultaneous GRAVITY image of S2 and Sgr A^{✻}. The image shows the central 150 mas (0.0059 pc ≈ 1.4 × 10^{4}R_{S}) after selfcalibration and CLEANing with AIPS. The image is reconstructed from 34 integrations of 5 min each from several nights at the end of March 2018. Sgr A^{✻} was (on average) K = 16.6 mag and the rms noise level of the background after cleaning is ≈20 mag. Both Sgr A^{✻} and S2 are unresolved. Here and in the other GRAVITY images, the elongation is due to the shape of the interferometric clean beam. Bottom: S2 – Sgr A^{✻} GRAVITY images (coaddition of several days) from July 2017 (bottom left) and May / June 2018, a few days after pericentre (bottom right). The inset in the bottom left panel shows the instantaneous interferometric beam, which is 2.2 mas × 4.7 mas without Earth rotation. The inset in the middle left shows a coadded SINFONI Kband spectrum of the star S2, taken from Habibi et al. (2017). 

In the text 
Fig. 2.
Summary of the observational results of monitoring the S2 – Sgr A^{✻} orbit from 1992 to 2018. Left: projected orbit of the star S2 on the sky (J2000) relative to the position of the compact radio source Sgr A^{✻} (brown crossed square at the origin). Triangles and circles (and 1σ uncertainties) denote the position measurements with SHARP at the NTT and NACO at the VLT, colourcoded for time (colour bar on the right side). All data points are corrected for the bestfit zeropoint (x_{0}; y_{0}) and drifts (ẋ_{0}, ẏ_{0}) of the coordinate system relative to Sgr A^{✻} (see Plewa et al. 2015). Green squares mark the GRAVITY measurements. The bottom right panel shows a zoom around pericentre in 2018. Top right: radial velocity of S2 as a function of time (squares: SINFONI/NACO at the VLT; triangles: NIRC2 at Keck). S2 reached pericentre of its orbit at the end of April 2002, and then again on May 19th, 2018 (MJD 58257.67). The data before 2017 are taken from Ghez et al. (2008), Boehle et al. (2016), Chu et al. (2018), and Gillessen et al. (2017, 2009b). The 2017/2018 NACO/SINFONI and GRAVITY data are presented here for the first time. The cyan curve shows the bestfitting S2 orbit to all these data, including the effects of General and Special Relativity. 

In the text 
Fig. 3.
Residual velocity c z = c(z_{GR} − z_{K}) for the best fitting prior Keplerian K_{prior} (f = 0, grey) and the same orbit with f = 1 (red GR_{prior}). K_{prior} was constructed from all 1992–2018 astrometric data with NACO & GRAVITY and the SINFONI data between 2004 and 2016 (open black circles). The 2017/2018 SINFONI data points (black circles with cyan shading) can then be added to test if the spectroscopic data around pericentre follow Kprior or the GR_{prior} predicted from K_{prior}. The new data points near and up to pericentre, where the β^{2} effects in radial velocity are expected to be important, fall close to the predicted GRprior curve, and exclude the Keplerian prior orbit. 

In the text 
Fig. 4.
Posterior analysis of all data by fitting for f simultaneously with all other parameters. We plot the residuals in spectroscopy (top, NIRC2, NACO, and SINFONI), Dec and RA (middle two panels, filled grey: NACO; open grey: SHARP; green filled blue: GRAVITY) between the best f = 1 fit and the f = 0 (Newtonian) part of that fit for the model (red line) and all data. The black curve includes the Schwarzschild precession. Here, we downsampled the NACO data into 100 equal bins along the orbit to obtain a constant weighting in spatial coverage. With a weight of 0.5 for the NACO data (in order to account for the systematic errors), this yields a 10 σ result in favour of GR (f = 0.90 ± 0.09), and . The bottom panel shows the posterior probability distributions for f and its correlation with the mass M_{•} and distance R_{0} of the massive black hole, and the argument of periapsis ω. The distributions are compact and all parameters are well determined. 

In the text 
Fig. A.1.
Posterior probability distributions obtained from a Markov chain for the 14parameter fit including f as a free parameter. All parameters are well constrained, in particular also f . We have omitted the panels corresponding to the four coordinate system parameters in this figure for clarity. 

In the text 
Fig. A.2.
Comparison of tests of General Relativity, inspired by Psaltis (2004). Shown in black are wellestablished tests: the Pound & Rebka (1959) experiment, the precession of Mercury (Einstein 1916), light deflection and the Shapiro delay in the solar system, the HulseTaylor pulsar (Taylor & Weisberg 1982), the gravitational redshift of Sirius B (Greenstein et al. 1971; Barstow et al. 2005), the LIGO detections (Abbott et al. 2016a,c,b), and the relativistic Fe Kα line (Tanaka et al. 1995; Fabian et al. 2000). Future tests are shown in grey, and this work, which uses the S2 orbit around Sgr A^{✻}, is shown in blue. 

In the text 
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