$\bf{<4.8}$ 
95 
^{ 1} 

CMS 
$\bf{<0.00016}$ 
95 
^{ 2} 


• • • We do not use the following data for averages, fits, limits, etc. • • • 
$<8.0$ 
95 
^{ 3} 

ATLS 
$<89$ 
95 
^{ 4} 

CMS 


^{ 5} 

CMS 
$<90$ 
95 
^{ 6} 

ATLS 


^{ 7} 

CMS 


^{ 8} 

ATLS 
$<127$ 
95 
^{ 9} 

ATLS 
$<34.4$ 
95 
^{ 10} 

ATLS 
$<0.0087$ 
95 
^{ 11} 

FLAT 
$<245$ 
95 
^{ 12} 

CDF 
$<615$ 
95 
^{ 13} 

D0 
$<0.916$ 
95 
^{ 14} 


$<350$ 
95 
^{ 15} 

CDF 
$<270$ 
95 
^{ 16} 

DLPH 
$<210$ 
95 
^{ 17} 

L3 
$<480$ 
95 
^{ 18} 

CDF 
$<0.00038$ 
95 
^{ 19} 


$<610$ 
95 
^{ 20} 

D0 
$<0.96$ 
95 
^{ 21} 


$<0.096$ 
95 
^{ 22} 


$<0.051$ 
95 
^{ 23} 


$<300$ 
95 
^{ 24} 

ALEP 


^{ 25} 


$<0.66$ 
95 
^{ 26} 




^{ 27} 


$<1300$ 
95 
^{ 28} 

L3 
^{1}
SIRUNYAN 2018S search for ${{\mathit p}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit j}}{{\mathit G}}$ , using 35.9 fb${}^{1}$ of data at $\sqrt {s }$ = 13 TeV to place lower limits on ${{\mathit M}_{{D}}}$ for two to six extra dimensions (see their Table VII), from which this bound on ${{\mathit R}}$ is derived. This limit supersedes that in KHACHATRYAN 2015AL.

^{2}
HANNESTAD 2003 obtain a limit on $\mathit R$ from the heating of old neutron stars by the surrounding cloud of trapped KK gravitons. Limits for all $\delta {}\leq{}$7 are given in their Tables$~$V and VI. These limits supersede those in HANNESTAD 2002 .

^{3}
AABOUD 2018I search for ${{\mathit p}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit j}}{{\mathit G}}$ , using 36.1 fb${}^{1}$ of data at $\sqrt {s }$ = 13 TeV to place lower limits on ${{\mathit M}_{{D}}}$ for two to six extra dimensions (see their Table 7), from which this bound on ${{\mathit R}}$ is derived. This limit supersedes that in AABOUD 2016D.

^{4}
SIRUNYAN 2018BV search for ${{\mathit p}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit Z}}{{\mathit G}}$ , using 35.9 fb${}^{1}$ of data at $\sqrt {s }$ = 13 TeV to place lower limits on ${{\mathit M}_{{D}}}$ for two to seven extra dimensions (see their Figure 11), from which this bound on R is derived.

^{5}
SIRUNYAN 2017AQ search for ${{\mathit p}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit G}}$ , using 12.9 fb${}^{1}$ of data at $\sqrt {s }$ = 13 TeV to place limits on ${{\mathit M}_{{D}}}$ for three to six extra dimensions (see their Table 3).

^{6}
AABOUD 2016F search for ${{\mathit p}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit G}}$ , using 3.2 fb${}^{1}$ of data at $\sqrt {s }$ = 13 TeV to place limits on ${{\mathit M}_{{D}}}$ for two to six extra dimensions (see their Figure 9), from which this bound on ${{\mathit R}}$ is derived.

^{7}
KHACHATRYAN 2016N search for ${{\mathit p}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit G}}$ , using 19.6 fb${}^{1}$ of data at $\sqrt {s }$ = 8 TeV to place limits on ${{\mathit M}_{{D}}}$ for three to six extra dimensions (see their Table 5).

^{8}
AAD 2015CS search for ${{\mathit p}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit G}}$ , using 20.3 fb${}^{1}$ of data at $\sqrt {s }$ = 8 TeV to place lower limits on ${{\mathit M}_{{D}}}$ for two to six extra dimensions (see their Fig. 18).

^{9}
AAD 2013C search for ${{\mathit p}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit G}}$ , using 4.6 fb${}^{1}$ of data at $\sqrt {s }$ = 7 TeV to place bounds on ${{\mathit M}_{{D}}}$ for two to six extra dimensions, from which this bound on ${{\mathit R}}$ is derived.

^{10}
AAD 2013D search for the dijet decay of quantum black holes in 4.8 fb${}^{1}$ of data produced in ${{\mathit p}}{{\mathit p}}$ collisions at $\sqrt {s }$ = 7 TeV to place bounds on ${{\mathit M}_{{D}}}$ for two to seven extra dimensions, from which these bounds on ${{\mathit R}}$ are derived. Limits on ${{\mathit M}_{{D}}}$ for all $\delta $ ${}\leq{}$ 7 are given in their Table 3.

^{11}
AJELLO 2012 obtain a limit on ${{\mathit R}}$ from the gammaray emission of point ${{\mathit \gamma}}$ sources that arise from the photon decay of KK gravitons which are gravitationally bound around neutron stars. Limits for all ${{\mathit \delta}}{}\leq{}$ 7 are given in their Table 7.

^{12}
AALTONEN 2008AC search for ${{\mathit p}}$ ${{\overline{\mathit p}}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit G}}$ and ${{\mathit p}}$ ${{\overline{\mathit p}}}$ $\rightarrow$ ${{\mathit j}}{{\mathit G}}$ at $\sqrt {s }$ = 1.96 TeV with 2.0 fb${}^{1}$ and 1.1 fb${}^{1}$ respectively, in order to place bounds on the fundamental scale and size of the extra dimensions. See their Table III for limits on all $\delta {}\leq{}$ 6.

^{13}
ABAZOV 2008S search for ${{\mathit p}}$ ${{\overline{\mathit p}}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit G}}$ , using 1 fb${}^{1}$ of data at $\sqrt {s }$ = 1.96 TeV to place bounds on ${{\mathit M}_{{D}}}$ for two to eight extra dimensions, from which these bounds on $\mathit R$ are derived. See their paper for intermediate values of $\delta $.

^{14}
DAS 2008 obtain a limit on $\mathit R$ from KaluzaKlein graviton cooling of SN1987A due to plasmonplasmon annihilation.

^{15}
ABULENCIA,A 2006 search for ${{\mathit p}}$ ${{\overline{\mathit p}}}$ $\rightarrow$ ${{\mathit j}}{{\mathit G}}$ using 368 pb${}^{1}$ of data at $\sqrt {s }$ = 1.96 TeV. See their Table II for bounds for all $\delta $ ${}\leq{}$ 6.

^{16}
ABDALLAH 2005B search for ${{\mathit e}^{+}}$ ${{\mathit e}^{}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit G}}$ at $\sqrt {s }$ = $180  209$~GeV to place bounds on the size of extra dimensions and the fundamental scale. Limits for all $\delta $ ${}\leq{}$ 6 are given in their Table~6. These limits supersede those in ABREU 2000Z.

^{17}
ACHARD 2004E search for ${{\mathit e}^{+}}$ ${{\mathit e}^{}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit G}}$ at $\sqrt {s }$ = $189  209$~GeV to place bounds on the size of extra dimensions and the fundamental scale. See their Table~8 for limits with $\delta $ ${}\leq{}$ 8. These limits supersede those in ACCIARRI 1999R.

^{18}
ACOSTA 2004C search for ${{\overline{\mathit p}}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit j}}{{\mathit G}}$ at $\sqrt {s }$ = 1.8~TeV to place bounds on the size of extra dimensions and the fundamental scale. See their paper for bounds on $\delta $~=~4,~6.

^{19}
CASSE 2004 obtain a limit on $\mathit R$ from the gammaray emission of point ${{\mathit \gamma}}$ sources that arises from the photon decay of gravitons around newly born neutron stars, applying the technique of HANNESTAD 2003 to neutron stars in the galactic bulge. Limits for all $\delta {}\leq{}$7 are given in their Table~I.

^{20}
ABAZOV 2003 search for ${{\mathit p}}$ ${{\overline{\mathit p}}}$ $\rightarrow$ ${{\mathit j}}{{\mathit G}}$ at $\sqrt {\mathit s }$=1.8 TeV to place bounds on $\mathit M_{\mathit D}$ for 2 to 7 extra dimensions, from which these bounds on $\mathit R$ are derived. See their paper for bounds on intermediate values of $\delta $. We quote results without the approximate NLO scaling introduced in the paper.

^{21}
HANNESTAD 2003 obtain a limit on $\mathit R$ from graviton cooling of supernova SN1987a. Limits for all $\delta {}\leq{}$7 are given in their Tables$~$V and VI.

^{22}
HANNESTAD 2003 obtain a limit on $\mathit R$ from gravitons emitted in supernovae and which subsequently decay, contaminating the diffuse cosmic$~{{\mathit \gamma}}$ background. Limits for all $\delta {}\leq{}$7 are given in their Tables$~$V and VI. These limits supersede those in HANNESTAD 2002 .

^{23}
HANNESTAD 2003 obtain a limit on $\mathit R$ from gravitons emitted in two recent supernovae and which subsequently decay, creating point$~{{\mathit \gamma}}$ sources. Limits for all $\delta {}\leq{}$7 are given in their Tables$~$V and VI. These limits are corrected in the published erratum.

^{24}
HEISTER 2003C use the process ${{\mathit e}^{+}}$ ${{\mathit e}^{}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit G}}$ at $\sqrt {\mathit s }$ = $189  209$ GeV to place bounds on the size of extra dimensions and the scale of gravity. See their Table$~$4 for limits with $\delta {}\leq{}$6 for derived limits on $\mathit M_{\mathit D}$.

^{25}
FAIRBAIRN 2001 obtains bounds on $\mathit R$ from over production of KK gravitons in the early universe. Bounds are quoted in paper in terms of fundamental scale of gravity. Bounds depend strongly on temperature of QCD phase transition and range from $\mathit R<0.13~\mu $m to $0.001~\mu $m for $\delta $=2; bounds for $\delta $=3,4 can be derived from Table$~$1 in the paper.

^{26}
HANHART 2001 obtain bounds on $\mathit R$ from limits on graviton cooling of supernova SN$~$1987a using numerical simulations of protoneutron star neutrino emission.

^{27}
CASSISI 2000 obtain rough bounds on $\mathit M_{\mathit D}$ (and thus $\mathit R$) from red giant cooling for $\delta $=2,3. See their paper for details.

^{28}
ACCIARRI 1999S search for ${{\mathit e}^{+}}$ ${{\mathit e}^{}}$ $\rightarrow$ ${{\mathit Z}}{{\mathit G}}$ at $\sqrt {\mathit s }$=189 GeV. Limits on the gravity scale are found in their Table$~$2, for $\delta {}\leq{}$4.
