Extremely energetic Fermi gamma-ray bursts obey spectral energy correlations

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Table 1:

The 25 GRBs with known redshift and measured $\ensuremath {E_{\rm p,i}}$ added to the sample of Amati et al. (2008) in our analysis of the $E_{\rm p,i}$ - $E_{\rm iso}$ correlation, providing a total of 95 GRBs.
GRB	z^a	$\ensuremath {E_{\rm p,i}}$	$\ensuremath {E_{\rm iso}}$ ^b	Instrument^c	Ref.^d
		[keV]	[ 10⁵² erg]
020127	1.9	290 $\pm$ 100	3.5 $\pm$ 0.1	HET	(1)
071003	1.604	2077 $\pm$ 286	36 $\pm$ 4	KW	(2)
080413	2.433	584 $\pm$ 180	8.1 $\pm$ 2.0	BAT/WAM	(3)
080413B	1.10	150 $\pm$ 30	2.4 $\pm$ 0.3	BAT	(4)
080514B	1.8	627 $\pm$ 65	17 $\pm$ 4	KW	(5)
080603B	2.69	376 $\pm$ 100	11 $\pm$ 1	KW	(6)
080605	1.6398	650 $\pm$ 55	24 $\pm$ 2	KW	(7)
080607	3.036	1691 $\pm$ 226	188 $\pm$ 10	KW	(8)
080721	2.591	1741 $\pm$ 227	126 $\pm$ 22	KW	(9)
080810	3.35	1470 $\pm$ 180	45 $\pm$ 5	GBM	(10)
080913	6.695	710 $\pm$ 350	8.6 $\pm$ 2.5	BAT/KW	(11)
080916	0.689	184 $\pm$ 18	1.0 $\pm$ 0.1	BAT/GBM^e	(12)
081007	0.5295	61 $\pm$ 15	0.16 $\pm$ 0.03	GBM	(13)
081008	1.9685	261 $\pm$ 52	9.5 $\pm$ 0.9	BAT	(14)
081028	3.038	234 $\pm$ 93	17 $\pm$ 2	BAT	(15)
081118	2.58	147 $\pm$ 14	4.3 $\pm$ 0.9	BAT/GBM $^{\it e}$	(16)
081121	2.512	871 $\pm$ 123	26 $\pm$ 5	KW	(17)
081222	2.77	505 $\pm$ 34	30 $\pm$ 3	GBM	(18)
090102	1.547	1149 $\pm$ 166	22 $\pm$ 4	KW	(19)
090328	0.736	1028 $\pm$ 312	13 $\pm$ 3	KW	(20)
090418	1.608	1567 $\pm$ 384	16 $\pm$ 4	BAT/KW	(21)
090423	8.1	491 $\pm$ 200	11 $\pm$ 3	GBM	(22)
090424	0.544	273 $\pm$ 50	4.6 $\pm$ 0.9	GBM	(23)
080916C	4.35	2646 $\pm$ 566	380 $\pm$ 80	GBM/KW	(24)
090323	3.57	1901 $\pm$ 343	410 $\pm$ 50	KW	(24)

^a Taken from the GRB table by J. Greiner and references therein (http://www.mpe.mpg.de/jcg/grbgen.html).
^b Computed in the 1-10 000 keV cosmological rest-frame by assuming a standard $\Lambda$ CDM cosmology with H₀= 70 km s^-1 Mpc^-1, $\Omega_{\rm M}$ = 0.27 and $\Omega_{\Lambda}$ = 0.73.
^c Instrument(s) that provided the spectral parameters and fluence used for the computation of $\ensuremath {E_{\rm p,i}}$ and $\ensuremath {E_{\rm iso}}$ : HET = HETE-2; BAT = Swift/BAT; KW = Konus/WIND; WAM = Suzaku/WAM; GBM = Fermi/GBM.
^d References for spectral parameters and fluence: (1) Sakamoto et al. (2005); (2) Golenetskii et al. (2007); (3) Ohno et al. (2008); (4) Barthelmy et al. (2008a); (5) Golenetskii et al. (2008a); (6) Golenetskii et al. (2008b); (7) Golenetskii et al. (2008c); (8) Golenetskii et al. (2008d); (9) Golenetskii et al. (2008e); (10) Meegan et al. (2008); (11) Palshin et al. (2008); (12) Bissaldi et al. (2008a) and Baumgartner et al. (2008); (13) Bissaldi et al. (2008b); (14) Palmer et al. (2008a); (15) Barthelmy et al. (2008b); (16) Palmer et al. (2008b) and Bhat et al. (2008); (17) Golenetskii et al. (2008g); (18) Bissaldi & McBreen (2008); (19) Golenetskii et al. (2009a); (20) Golenetskii et al. (2009c); (21) Palshin et al. (2009); (22) von Kienlin (2009); (23) Connaughton (2009); (24) see text.
^e Spectral parameters from Fermi/GBM and fluence from Swift/BAT.

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