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Appendix A: Absolute B magnitudes of GRB host galaxies

The dereddened R magnitudes of the GRB host galaxies with determined redshifts are given in Table .1. They were estimated in the Vega system taking account of most of the published papers and GRB Coordinates Network circulars directly or indirectly reporting on optical observations of fading GRB afterglows and their hosts. When several R magnitudes of a given source were available in the literature, the various measurements were weighted according to their photometric uncertainty, and subsequently averaged to get a final homogenized value. In some cases, we also relied on the host contribution derived from the fit of the R-band optical transient light-curve when the latter was clearly well constrained. The Rmagnitude of the GRB 990506 host galaxy was measured from an R-band image that we obtained using the EFOSC2 instrument on the ESO 3.6-m telescope at La Silla.

 

 

Table A.1: Optical (R and B-band) properties of GRB host galaxies.

		Redshift			Photometry				$M_B + 5 \log_{10} h_{65}~(\P)$
Source	GRB	z	Ref.		$E(B-V)^{\dag }$	R mag	References		(1)	(2)
GRB J194641.9-193605	020813	1.25	1		0.109	24.70 $\pm$ 0.20	2		-19.30
GRB J151455.8-192454	020531	1.00	3		0.140	22.05 $\pm$ 0.20	4		-21.35
GRB J135803.1-312222	020405	0.69	5		0.050	20.90 $\pm$ 0.20	5		-21.50
GRB J111518.0-215656	011211	2.14	6		0.036	24.90 $\pm$ 0.30	7		-20.55
GRB J113429.6-760141	011121	0.36	8		0.508	24.60 $\pm$ 0.40	9		-16.15	-16.25
GRB J225559.9+405553	010921	0.45	10		0.145	21.45 $\pm$ 0.15	10, 11		-19.75	-19.95
GRB J145212.5+430106	010222	1.48	12		0.023	25.70 $\pm$ 0.15	13, 14		-18.75	-18.50
GRB J170409.7+514711	000926	2.04	15		0.024	24.80 $\pm$ 0.10	15		-20.50
GRB J021834.5+074429	000911	1.06	16		0.120	25.10 $\pm$ 0.10	16		-18.80	-18.85
GRB J122519.3+200611	000418	1.12	17		0.033	23.80 $\pm$ 0.20	18, 19		-19.90	-19.85
GRB J162018.6+292636	000301	2.04	20		0.052	27.85 $\pm$ 0.30	21		-17.45
GRB J015915.5-403933	000210	0.85	22		0.017	23.45 $\pm$ 0.10	22		-19.50	-19.50
GRB J050931.3+111707	991216	1.02	23		0.633	25.30 $\pm$ 0.20	24		-18.15
GRB J163353.5+462721	991208	0.71	25		0.016	24.30 $\pm$ 0.20	25, 26		-18.30	-18.30
GRB J223153.1-732429	990712	0.43	27		0.032	21.85 $\pm$ 0.15	28, 29, 30		-19.35	-19.50
GRB J050954.5-720753	990705	0.84	31		0.122	21.80 $\pm$ 0.10	31, 32, 33		-21.65	-21.75
GRB J133807.1-802948	990510	1.62	27		0.118	27.50 $\pm$ 0.30$^\ddag$	34		-17.20
GRB J115450.1-264035	990506	1.31	17		0.065	25.50 $\pm$ 0.20	this work		-19.75	-19.45
GRB J152530.3+444559	990123	1.60	35		0.016	24.30 $\pm$ 0.40	26, 36, 37, 38		-20.40	-20.05
GRB J235906.7+083507	980703	0.97	39		0.058	22.40 $\pm$ 0.20	26, 40, 41, 42		-20.90	-20.80
GRB J101757.8+712725	980613	1.10	43		0.090	25.80 $\pm$ 0.10	44		-17.85	-17.90
GRB J115626.4+651200	971214	3.42	45		0.016	25.60 $\pm$ 0.20	26, 45, 46		-21.30	-21.30
GRB J180831.6+591851	970828	0.96	47		0.038	25.10 $\pm$ 0.30	47		-18.85	-18.35
GRB J065349.4+791619	970508	0.83	48		0.049	25.10 $\pm$ 0.20	26, 48, 49		-17.85	-17.75
GRB J050146.7+114654	970228	0.69	50		0.234	24.60 $\pm$ 0.20	50, 51, 52		-17.85	-17.80

Notes:
$\dag$ Foreground Galactic extinction. For all cases excepted GRB 990705, it has been estimated from the DIRBE/IRAS dust maps of Schlegel et al. (1998). For GRB 990705 which occured behind the Large Magellanic Cloud, we used the results of Dutra et al. (2001).
$\ddagger$ Derived from the V magnitude of Fruchter et al. (2000a) assuming a spectral slope $F_{\nu} \varpropto \nu^{-1}$.
$\P$ The absolute B magnitudes were derived assuming a $\Lambda$CDM Universe with $\Omega _m=0.3$ and $\Omega _\lambda =0.7$. Column (1) gives the estimations which were obtained by applying proper k-corrections and B-R colours to the observed R magnitudes. The results given in Col. (2) were derived from the observed flux density at the redshifted B-band wavelength.

References: (1) Price et al. (2002b); (2) Levan et al. (2002); (3) Kulkarni et al. (2002); (4) Fox et al. (2002); (5) Price et al. (2002d); (6) Holland et al. (2002); (7) Burud et al. (2001); (8) Garnavich et al. (2003); (9) Bloom et al. (2002c); (10) Price et al. (2002c); (11) Park et al. (2002); (12) Jha et al. (2001); (13) Frail et al. (2002); (14) Fruchter et al. (2001a); (15) Castro et al. (2002); (16) Price et al. (2002a); (17) Bloom et al. (2002a); (18) Metzger et al. (2000); (19) Klose et al. (2000); (20) Jensen et al. (2001); (21) Fruchter & Vreeswijk (2001); (22) Piro et al. (2002); (23) Vreeswijk et al. (1999b); (24) Vreeswijk et al. (2000); (25) Castro-Tirado et al. (2001); (26) Sokolov et al. (2001); (27) Vreeswijk et al. (2001); (28) Fruchter et al. (2000b); (29) Hjorth et al. (2000); (30) Sahu et al. (2000); (31) Le Floc'h et al. (2002); (32) Saracco et al. (2001a); (33) Holland et al. (2000a); (34) Fruchter et al. (2000a); (35) Kulkarni et al. (1999); (36) Fruchter et al. (1999b); (37) Holland & Hjorth (1999); (38) Bloom et al. (1999); (39) Djorgovski et al. (1998); (40) Bloom et al. (1998b); (41) Holland et al. (2001); (42) Vreeswijk et al. (1999a); (43) Djorgovski et al. (2000); (44) Hjorth et al. (2002); (45) Kulkarni et al. (1998); (46) Odewahn et al. (1998); (47) Djorgovski et al. (2001); (48) Bloom et al. (1998a); (49) Fruchter et al. (2000c); (50) Bloom et al. (2001); (51) Fruchter et al. (1999a); (52) Galama et al. (2000).

The redshifts given in Table .1 have also been taken from the literature. In most cases, they were determined from emission lines directly observed in the spectra of the hosts. For the other sources, they were derived as the redshifts of the furthest absorbing medium observed in absorption within the spectra of the GRB optical transients. We made the assumption that the first interstellar medium illuminated by the background afterglow is indeed that of its host galaxy itself. We note that this hypothesis has been confirmed in several cases where the derived redshift could have been confirmed with emission lines from the host.

These redshifts and R magnitudes were subsequently used to derive the absolute B magnitudes given in Col. (1) of Table .1, assuming a $\Lambda$CDM Universe with $\Omega _m=0.3$, $\Omega _\lambda =0.7$. For each host, the k-correction for the R-filter and rest-frame B-R colour used for this computation were estimated taking account of the type of SED suggested by its R-K and/or optical colours when available (see Table 2 and Fig. 4), otherwise assuming a blue continuum with a spectral slope $F_{\nu} \varpropto \nu^{-1}$.

To better establish the validity of our results, we also estimated, for most of the hosts, the absolute B magnitudes from the observed flux density at the redshifted B-band wavelength. For each case, this flux density was derived interpolating the various broad-band filter magnitudes given in the literature (see Table .1 for references) including the K magnitudes given in Table 2. The final results are indicated in Col. (2) of Table .1. To compare the two methods, we computed the difference between the estimations given in the two columns, and found a mean value < M_B(1) - M_B(2) > = 0.07 and a dispersion $\sigma$  $\left(M_{B(1)}{-}M_{B(2)}\right)=0.18$.