graviton MASS INSPIRE search

Van Dam and Veltman (VANDAM 1970 ), Iwasaki (IWASAKI 1970 ), and Zakharov (ZAKHAROV 1970 ) almost simultanously showed that $\ldots$ there is a discrete difference between the theory with zero-mass and a theory with finite mass, no matter how small as compared to all external momenta.'' The resolution of this "vDVZ discontinuity" has to do with whether the linear approximation is valid. De Rham $\mathit et\mathit al.$ (DE-RHAM 2011 ) have shown that nonlinear effects not captured in their linear treatment can give rise to a screening mechanism, allowing for massive gravity theories. See also GOLDHABER 2010 and DE-RHAM 2017 and references therein. Experimental limits have been set based on a Yukawa potential or signal dispersion. $\mathit h_{0}$ is the Hubble constant in units of 100 km$~$s${}^{-1}~$Mpc${}^{-1}$.

The following conversions are useful: 1 eV = $1.783 \times 10^{-33}$ g = $1.957 \times 10^{-6}{\mathit m}_{{{\mathit e}}}$; $ƛ_{C}$ = ($1.973 \times 10^{-7}$ m)${\times }$(1 eV/${\mathit m}_{{{\mathit g}}}$).
VALUE (eV) DOCUMENT ID TECN  COMMENT
$\bf{<6 \times 10^{-32}}$ 1
 2004
YUKA Weak gravitational lensing
• • • We do not use the following data for averages, fits, limits, etc. • • •
$<7 \times 10^{-23}$ 2
 2017
DISP Combined dispersion limit from three BH mergers
$<1.2 \times 10^{-22}$ 2
 2016
DISP Combined dispersion limit from two BH mergers
$<5 \times 10^{-23}$ 3
 2013
Spinning black holes bounds
$<4 \times 10^{-25}$ 4
 2008
Graviton phase velocity fluctuations
$<6 \times 10^{-32}$ 5
 2005
YUKA Solar System observations
$<9.0 \times 10^{-34}$ 6
 2004
From $\Omega _{tot}$ value assuming RTG
$>6 \times 10^{-34}$ 7
 2003
Horizon scales
$<8 \times 10^{-20}$ 8, 9
 2002
DISP Binary pulsar orbital period decrease
10, 9
 1991
Binary pulsar PSR 1913$+$16
$<7 \times 10^{-23}$
 1988
YUKA Solar system planetary astrometric data
$<2 \times 10^{-29} \mathit h{}^{-1}_{0}$
 1974
Rich clusters
$<7 \times 10^{-28}$
 1973
Galaxy
$<8 \times 10^{4}$
 1973
2${{\mathit \gamma}}$ decay
1  CHOUDHURY 2004 concludes from a study of weak-lensing data that masses heavier than about the inverse of 100 Mpc seem to be ruled out if the gravitation field has the Yukawa form.
2  ABBOTT 2016 and ABBOTT 2017 assumed a dispersion relation for gravitational waves modified relative to GR.
3  BRITO 2013 explore massive graviton (spin-2) fluctuations around rotating black holes.
4  BASKARAN 2008 consider fluctuations in pulsar timing due to photon interactions (surfing'') with background gravitational waves.
5  GRUZINOV 2005 uses the DGP model (DVALI 2000 ) showing that non-perturbative effects restore continuity with Einstein's equations as the gravition mass approaches 0, then bases his limit on Solar System observations.
6  GERSHTEIN 2004 use non-Einstein field relativistic theory of gravity (RTG), with a massive graviton, to obtain the 95$\%$ CL mass limit implied by the value of $\Omega _{tot}$ = $1.02$ $\pm0.02$ current at the time of publication.
7  DVALI 2003 suggest scale of horizon distance via DGP model (DVALI 2000 ). For a horizon distance of $3 \times 10^{26}$ m (about age of Universe/$\mathit c$; GOLDHABER 2010 ) this graviton mass limit is implied.
8  FINN 2002 analyze the orbital decay rates of PSR$~$B1913+16 and PSR$~$B1534+12 with a possible graviton mass as a parameter. The combined frequentist mass limit is at 90$\%$CL.
9  As of 2014, limits on dP/dt are now about 0.1$\%$ (see T. Damour, Experimental tests of gravitational theory,'' in this $\mathit Review$).
10  DAMOUR 1991 is an analysis of the orbital period change in binary pulsar PSR$~1913+$16, and confirms the general relativity prediction to $0.8\%$. The theoretical importance of the [rate of orbital period decay] measurement has long been recognized as a direct confirmation that the gravitational interaction propagates with velocity $\mathit c$ (which is the immediate cause of the appearance of a damping force in the binary pulsar system) and thereby as a test of the existence of gravitational radiation and of its quadrupolar nature.'' TAYLOR 1993 adds that orbital parameter studies now agree with general relativity to $0.5\%$, and set limits on the level of scalar contribution in the context of a family of tensor [spin$~$2]-biscalar theories.
References:
 ABBOTT 2017
PRL 118 221101 GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2
 ABBOTT 2016
PRL 116 061102 Observation of Gravitational Waves from a Binary Black Hole Merger
 BRITO 2013
PR D88 023514 Massive Spin-2 Fields on Black Hole Spacetimes: Instability of the Schwarzschild and Kerr Solutions and Bounds on the Graviton Mass
PR D78 044018 Limits on the Speed of Gravitational Waves from Pulsar Timing
 GRUZINOV 2005
NAST 10 311 On the Graviton Mass
 CHOUDHURY 2004
ASP 21 559 Probing Large Distance Higher Dimensional Gravity from Lensing Data
 GERSHTEIN 2004
PAN 67 1596 Graviton Mass, Quintessence and Oscillatory Character of the Universe Evolution
 DVALI 2003
PR D68 024012 The Accelerated Universe and the Moon
 FINN 2002
PR D65 044022 Bounding the Mass of the Graviton using Binary Pulsar Observations
 DAMOUR 1991
APJ 366 501 On the Orbital Period Change of the Binary Pulsar PSR B1913+16
PRL 61 1159 Model Independent Constraints on Possible Modifications of Newtonian Gravity
 GOLDHABER 1974
PR D9 1119 Mass of the Graviton
 HARE 1973
CJP 51 431 Mass of the Graviton
 TAYLOR 1993
NAT 355 132 Experimental Constraints on Strong Field Relativistic Gravity
 ABBOTT 2017L
NAT 551 85 A Gravitational-wave Standard Siren Measurement of the Hubble Constant
 GOLDHABER 2010
RMP 82 939 Photon and Graviton Mass Limits
 DVALI 2000
PL B485 208 4D Gravity on a Brane in 5D Minkowski Space
 VANDAM 1970
NP B22 397 Massive and Mass-Less Yang-Mills and Gravitational Fields
 IWASAKI 1970
PR D2 2255 Consistency Condition for Propagators
 ZAKHAROV 1970
JETPL 12 312 Linearized Gravitation Theory and the Graviton Mass
 DE-RHAM 2017
RMP 89 025004 Graviton Mass Bounds
 DE-RHAM 2011
PRL 106 231101 Resummation of Massive Gravity