Vesna Borka Jovanović "Constraining Scalar-Tensor gravity models by S2 star orbits around the Galactic Center"

V. Borka Jovanović1, P. Jovanović2, D. Borka1,
S. Capozziello3,4,5, S. Gravina3, A. D'Addio3
1Atomic Physics Laboratory (040), Vinča Institute of Nuclear Sciences,
P.O. Box 522, 11001 Belgrade, Serbia
2Astronomical Observatory, Volgina 7, P.O. Box 74, 11160 Belgrade,
Serbia
3Dipartimento di Fisica, Università di Napoli ''Federico II'', Napoli, Italy
4INFN - Sezione di Napoli, Via Cinthia, I-80126, Napoli, Italy
5Gran Sasso Science Institute, Viale F. Crispi, 7, I-67100, L'Aquila, Italy
Constraining Scalar-Tensor gravity
models by S2 star orbits
around the Galactic Center

Borka Jovanović et al.2 BW2018
Outline of the talk
 Object and goal: to test Scalar-Tensor (ST) gravity models using
kinematics of S-like stars
 Motivation: using ST gravity, as well as the other modifications of
standard Einstein's gravity, some observed phenomena may be explained
without dark matter and dark energy
 Data: NTT/VLT telescope, Gillessen et al., ApJ 692, 1075 (2009)
 Method: ST is analyzed using observed orbits of S-stars around Galactic
Center and also using two-body simulations
 Results: we review the various consequences of the ST gravity
parameters on stellar dynamics and investigate their constraints from the
observed S-star orbits
 Conclusions
 References

Modified gravity and rotation curves of spiral
galaxies
tekst
Sofue & Rubin, 2001,
ARA&A, 39, 137
NGC 1560
Newtonian
prediction
observation observed
Capozziello et al. 2007,
MNRAS, 375, 1423
Rn gravity: β = 0.817; n = 3.5

Scalar-Tensor (ST) theory of gravity
- both the metric tensor gμν and a fundamental scalar field φ are involved
- it contains two arbitrary functions of the scalar field: the coupling F(φ)φ)
and the interaction potential V(φ)φ)
F(φ)φ) – underlines a non-minimal coupling between the scalar field
and the geometry
V(φ)φ) – implies a self-interaction of the field
In our study we take the action of the form:
We choose a specific form for F(φ)φ) = ξφm, V(φ)φ) = λφn, where ξ is a
coupling constant, λ gives the self-interaction potential strength, m and n
are arbitrary parameters (S. Capozziello, R. de Ritis, C. Rubano, P.
Scudellaro, La Rivista del Nuovo Cimento 19, 1 (1996)).

Parameters of ST gravity
The ST gravitational potential in the weak field limit can be written in the
form (D'Addio et al. 2018 & Gravina et al. 2018, in Publ. AOB):
Parameters:
ξ - a coupling constant
λ - parameter which gives the self-interaction potential strength
m,n - arbitrary integer numbers, for which it stands: n ≠ 2m, n ≠ 0
p - function of the ST gravity parameters ξ, λ, m, n
φ0 - positive real number, close to 1
In order to constrain these parameters observationally, we simulated orbits of
S2 star in the modified gravitational potential, and then we compared the
results with the set of S2 star observations obtained by the Very Large
Telescope (VLT).

S2 star orbits in ST and Newtonian potential
- we compare the obtained theoretical results for S2-like star orbits in the
ST potential with the available set of observations of the S2 star
- we draw orbits of S2 star in ST and Newtonian potential.
Modified: ΦST(r) = C1·(1/r) + C2·r2 + C3·exp(-p·r)/r
C1 = C1(ξ, m), C2 = C2(ξ, λ, m, n), C3 = C3(ξ, m), p = p(ξ, λ, m, n)
Newton: ΦN(r) = – GM/r
The massive black hole Sgr A* at the Galactic center
is surrounded by a cluster of stars orbiting around it:
S-star cluster.
S2 star is one of the brightest among S-stars, with the
short orbital period and the smallest uncertainties in
determining the orbital parameters: a good candidate
for this study.

Observations and method
- observations collected between 1992 and 2008 at the ESO (European
Southern Observatory): NTT/VLT optical telescopes
- data publicly available as the supplementary online data to the electronic
version of paper Gillessen et al., ApJ 692, 1075 (2009)
New
Technology
Telescope
(3.6 m)
La Silla
Observatory,
Chile
Very Large
Telescope
(4 x 8.2 m)
Paranal
Observatory,
Chile
- we performed two-body simulations in the ST gravity potential

Results I: simulated orbits of S2 star in ST gravity
Comparison between the orbit of S2
star in Newtonian and ST potential
during t = 2 T, t = 10 T and more orbital
periods (t = 45, 90, 120 and 180 T).
- positive precession (as in GR)
- prograde shift that results in rosette-
shaped orbits

Results II: comparison between the simulated
and observed orbits of S2 star
m = 2, n = 3
- we calculate the positions of S2
star in the orbital plane (the true
orbit) by the numerical integration
of equations of motion
- then we project the true orbit to
the observed plane (the apparent
orbit)
- discrepancy between the
simulated and the observed
apparent orbit is estimated by the
reduced χ2

Results III: orbital precession
The comparison of the fitted orbit of S2 star and astrometric observations:
(m,n) = (2,3) and (ξ,λ)=(-1000, 0.0006).
orbital
precession

Results IVa: constraints on ST gravity parameters
The map of the reduced χ2 over the parameter space (ξ,λ) of ST gravity.
- for chosen:
φ0 = 1
m = 1, n = 4,
parameters of the
best fit are:
χ2min = 1.54
ξ_minmin = 43000
λ_minmin = -0.0024
- we chose some values for (m,n), and vary the parameters (ξ,λ) over some
intervals, and search for those solutions which for the simulated orbits in
ST gravity give at least the same (χ2 =1.89) or better fits (χ2 <1.89) than
the Keplerian orbits
- we repeat the procedure for different combinations (m,n) → [1,10]

Results IVb: constraints on ST gravity parameters
(m,n) = (3,4) χ2min = 1.54; ξ_minmin = 1000; λ_minmin = 0.0005
Note: χ2min – minimal value
ξ_minmin, λ_minmin – not minimal, but the most probable values

IVc: constraints on ST gravity parameters
(m,n) = (4,4)
χ2min = 1.54;
ξ_minmin = 15000; λ_minmin = 0.0067
(m,n) = (10,10)
χ2min = 1.54;
ξ_minmin = -15000; λ_minmin = -0.0067
m = n:
ξ_minmin,1 = ξ_minmin,2, λ_minmin,1 = λ_minmin,2

Results V: best fit values for ST gravity parameters
With the parameter space
{ξ,λ} determined in this way,
we calculate the simulated
orbits, and then compare them
with the observations.
In that way, our results enable
us to test Scalar Tensor
Theory at galactic scales.
φ0 = 1
(m,n) → [1,10] n ≠ 2m
χ2 m n ξ λ
1.5434350 1 1 13000 0.0058
1.5434440 1 3 43000 -0.0064
1.5434426 1 4 43000 -0.0024
1.5434345 2 1 16000 0.0095
1.5434352 2 2 15000 0.0067
1.5434474 2 3 -1000 -0.0006
1.5434336 3 1 1000 0.0008
1.5434383 3 2 1000 0.0005
1.5434352 3 3 15000 0.0067
1.5434383 3 4 1000 0.0005
1.5434317 4 1 4000 0.0041
1.5434478 4 2 -1000 -0.0006
1.5434348 4 3 21000 0.0100
1.5434353 4 4 15000 0.0067
... ... ...
1.5434353 10 10 -15000 -0.0067

Conslusions
✔ We derived a particular theory among the class of Scalar Tensor theories
of gravity, and then tested it by studying dynamics of S2 star around
supermassive black hole at Galactic Center.
✔ Using the observed positions of S2 star around the GC, we constrained
the parameters of ST gravitational potential.
✔ To constrain these parameters, we compare the observed orbit of S2 star
with our simulated orbit which we obtained theoretically with the derived
potential.
✔ We obtained the most probable values for parameters λ and ξ, for
different parameters m and n, and they fit better astronomy data than
Keplerian orbit.

Conslusions II
✔ The precession of S2 star orbit obtained for the best fit parameter values
has the positive direction (as in General Relativity).
✔ We obtained much larger orbital precession of the S2 star in ST gravity
than the corresponding value predicted by general relativity.
✔ The approach we are proposing can be used to constrain the different
modified gravity models from stellar orbits around Galactic Center.

References
[1] S. Capozziello, G. Lambiase, M. Sakellariadou, A. Stabile, An. Stabile,
Phys. Rev. D 91, 044012 (2015).
[2] A. D’Addio, S. Capozziello, P. Jovanović, V. Borka Jovanović, Book of
abstracts of the XVIII Serbian Astronomical Conference, Belgrade, Serbia,
October 17-21, p. 34 (2017).
[3] S. Gravina, S. Capozziello, D. Borka, V. Borka Jovanović, Book of
abstracts of the XVIII Serbian Astronomical Conference, Belgrade, Serbia,
October 17-21, p. 40 (2017).
[4] A. D’Addio, S. Capozziello, P. Jovanović, V. Borka Jovanović, Publ.
Astron. Obs. Belgrade, in press (2018).
[5] S. Gravina, S. Capozziello, D. Borka, V. Borka Jovanović, Publ.
Astron. Obs. Belgrade, in press (2018).
[6] S. Gravina, Master Thesis "The Galactic Center as a gravitational
laboratory", University of Naples "Federico II", Italy, 2017.
[7] A. D'Addio, Master Thesis "Testing theories of gravity by Sgr A*",
University of Naples "Federico II", Italy, 2017.

References
[8] D. Borka, P. Jovanović, V. Borka Jovanović, A. F. Zakharov, Phys. Rev.
D 85, 124004-1-11 (2012).
[9] D. Borka, S. Capozziello, P. Jovanović, V. Borka Jovanović, Astropart.
Phys. 79, 41-48 (2016).
[10] A. F. Zakharov, P. Jovanović, D. Borka, V. Borka Jovanović, J.
Cosmol. Astropart. P. 5, 045-1-10 (2016).
[11] V. Borka Jovanović, S. Capozziello, P. Jovanović, D. Borka, Phys.
Dark Universe 14, 73-83 (2016).
[12] S. Capozziello, P. Jovanović, V. Borka Jovanović, D. Borka, J.
[13] 19. A. F. Zakharov, P. Jovanović, D. Borka, V. Borka Jovanović, J.

Vesna Borka Jovanović "Constraining Scalar-Tensor gravity models by S2 star orbits around the Galactic Center"

More Related Content

What's hot (16)

Similar to Vesna Borka Jovanović "Constraining Scalar-Tensor gravity models by S2 star orbits around the Galactic Center" (20)

More from SEENET-MTP (20)

Recently uploaded (20)

Vesna Borka Jovanović "Constraining Scalar-Tensor gravity models by S2 star orbits around the Galactic Center"