$\bf{<6 \times 10^{32}}$ 
^{ 1} 

YUKA 
• • • We do not use the following data for averages, fits, limits, etc. • • • 
$<7 \times 10^{23}$ 
^{ 2} 

DISP 
$<1.2 \times 10^{22}$ 
^{ 2} 

DISP 
$<5 \times 10^{23}$ 
^{ 3} 


$<4 \times 10^{25}$ 
^{ 4} 


$<6 \times 10^{32}$ 
^{ 5} 

YUKA 
$<9.0 \times 10^{34}$ 
^{ 6} 


$>6 \times 10^{34}$ 
^{ 7} 


$<8 \times 10^{20}$ 
^{ 8}^{, 9} 

DISP 

^{ 10}^{, 9} 


$<7 \times 10^{23}$ 


YUKA 
$<2 \times 10^{29} \mathit h{}^{1}_{0}$ 



$<7 \times 10^{28}$ 



$<8 \times 10^{4}$ 



^{1}
CHOUDHURY 2004 concludes from a study of weaklensing 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 (spin2) 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 nonperturbative 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 nonEinstein 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.
