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Observations of GRB host galaxies

The main goal of observations of GRB host galaxies is accumulation of statistics of their spectroscopic and photometric properties. These research activities help us, we believe, to shed light on the main problem of GRB astronomy - problem of progenitors.

To escape any systematic shifts of data from different instruments we observe the objects with one instrument (6-m telescope SAO RAS) and in the standard photometric system (Johnson-Kron-Cousins). Below we present first compilation of our data obtained for several GRB host galaxies. Photometric calibration of data was performed using Landolt and Stetson standards. All magnitudes are corrected for Galactic extinction. The last column includes information about spectroscopic observations of other authors: what kind of spectrum was obtained (emission or absorption), whether spectrum included contribution of OT or not, and what redshift value was derived.

As a result of this compilation we present here the Hubble diagram (redshift -- magnitude) for GRB host galaxies (see the caption of the figure).

The Hubble diagram for 22 GRB host galaxies with known magnitudes and redshifts (GRB 970228, GRB 970508, GRB 970828, GRB 971214, GRB 980613, GRB 980703, GRB 990123, GRB 990510, GRB 990712, GRB 9912008, GRB 991216, GRB 000131, GRB 000210, GRB 000301C, GRB 000418, GRB 000911, GRB 000926, GRB 001109, GRB 010222, GRB 010921, GRB 011121 and GRB011211).

By the dotes the results of photometric redshift estimates of Hubble Deep Field galaxies are presented. Original HDF AB magnitudes were transformed to the Vega ones using the following equation F606W(Vega) = F606W(AB)-0.12. Here we assumed that F606W band roughly corresponds to Cousins R band.


Photometry of GRB host galaxies with the 6-m telescope
 Host galaxy   Date UT  Band   Exp. 
 s 		  Dereddened 
 magnitude 		  Seeing   Spectrum 
 GRB 971214   24.85 Jul. 1998     V    600   25.43 +/- 0.30    1".2  emission host+OT (z=3.42)
(Kulkarni et al. 1998)
 24.84 Jul.      Rc    600   25.69 +/- 0.30    1".2 
 GRB 970508   21.74 Aug. 1998      B  4200   25.77 +/- 0.19    1".3 emission host+OT (z=0.835)
(Metzger et al. 1997,
Bloom et al. 1998)
 23.95 Jul. 1998     V  2000   25.25 +/- 0.22    1".3
 21.74 Aug.     Rc  3000   24.99 +/- 0.17    1".3
 23.95 Jul.     Ic  2000   24.07 +/- 0.25    1".3
 GRB 980613   24.80 Jul. 1998     B   700  24.77 +/- 0.25    1".3 emission host (z=1.096)
(Djorgovski et al. GCN #189)
 24.82 Jul.     V   600  23.94 +/- 0.21    1".3
 23.00 Jul.     Rc  1800  23.58 +/- 0.10    1".5
 GRB 980703   24.05 Jul. 1998     B   480  23.15 +/- 0.12    1".3 emission host+OT (z=0.966)
(Djorgovski et al. 1998)
 24.06 Jul.     V   320  22.66 +/- 0.10    1".2
 24.06 Jul.     Rc   300  22.30 +/- 0.08    1".2
 24.07 Jul.     Ic   360  22.17 +/- 0.18    1".2
 GRB 990123   8.85 Jul. 1999     B  600  24.90 +/- 0.16    1".5 absorption host+OT (z=1.6)
(Kelson et al. 1999,
Hjorth et al. 1999)
 8.86 Jul.     V  600  24.47 +/- 0.13    1".3
 8.84 Jul.     Rc  600  24.47 +/- 0.14    1".1
 8.87 Jul.     Ic  600  24.06 +/- 0.30    1".3
 GRB 991208   31.90 Mar. 2000     B  1795  25.18 +/- 0.16   3".0 emission host+OT (z=0.7063)
(Dodonov et al. GCN #475)
 31.84 Mar.     V  1490  24.63 +/- 0.16   2".1
 31.96 Mar.     Rc  1260  24.36 +/- 0.15   2".1
 31.87 Mar.     Ic   360  23.70 +/- 0.28   2".6
 GRB 000926   25 July 2001     B  2500  26.02 +/- 0.17   1".3 absorption host+OT (z=2.0369)
(Castro et al. GCN #851)
 25 July     V  1500  25.77 +/- 0.22   1".3
 24 July     Rc  1260  26.24 +/- 0.25   1".3
 25 July     Ic   1800  24.65 +/- 0.40   1".3
 GRB 001109                  emission host (z=0.398+/-0.002)
(Afanasiev et al. GCN #1090)
               
  24 July 2001     R    22.4 +/- 0.2   1.3"
  This     is   spec.   estimation    
Note: All magnitudes were corrected for Galactic extinction using curve from Cardelli, Clayton & Mathis 1989, ApJ, 345, 245

References:

  • Bloom J. S., Djorgovski S. G., Kulkarni S. R., Frail D. A., 1998, ApJ, 507, L25
  • Djorgovski S. G., Kulkarni S. R., Bloom J. S., Goodrich R., Frail D. A., Piro L., Palazzi E., 1998, ApJ, 508, L17
  • Hjorth J., et al. 1999, GCN Circ. 219
  • Kelson D. D., Illingworth G. D., Franx M., Magee D., & van Dokkum P. G., 1999, IAU Circ. 7096
  • Kulkarni S. R., Djorgovski S. G., Ramaprakash A. N., Goodrich R., Bloom J. S., Adelberger K. L., Kundic T., Lubin L., Frail D. A., Frontera F., Feroci M., Nicastro L., Barth A. J., Davis M., Filippenko A. V., 1998, Nature, 393, 35
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