Skip to main content Accessibility help

The Cosmic Evolution of Gamma-Ray Burst Host Galaxies

  • S. Savaglio (a1)


Due to their extreme luminosities, gamma-ray bursts (GRBs) can be detected in hostile regions of galaxies, nearby and at very high redshift, making them important cosmological probes. The investigation of galaxies hosting long-duration GRBs (whose progenitor is a massive star) demonstrated their connection to star formation. Still, the link to the total galaxy population is controversial, mainly because of the small-number statistics: ~1, 100 are the GRBs detected so far, ~280 those with measured redshift, and ~70 the hosts studied in detail. These are typically low-redshift (z < 1.5), low luminosity, metal poor, and star-forming galaxies. On the other hand, at 1.5 < z < 4, massive, metal rich and dusty, interacting galaxies are not uncommon. The most distant population (z > 4) is poorly explored, but the deep limits reached point towards very small and star-forming objects, similar to the low-z population. This “back to the future” behavior is a natural consequence of the connection of long GRBs to star formation in young regions of the universe.



Hide All
[1]Basa, S., Cuby, J.G., Savaglio, S., et al., 2012, A&A, 542, A103
[2]Berger, E., Chornock, R., Lunnan, R., et al., 2012, ApJ, 755, L29
[3]Bluck, A.F.L., Conselice, C.J., Buitrago, F., et al., 2012, ApJS, 747, 34
[4]Chen, H.-W., 2012, MNRAS, 419, 3039
[5]Christensen, L., Fynbo, J.P.U., Prochaska, J.X., et al., 2011, ApJ, 727, 73
[6]Cooke, J., Sullivan, M., Barton, E.J., et al., 2009, Nature, 460, 237
[7]Cooke, J., Berrier, J.C., Barton, E.J., et al., 2010, MNRAS, 403, 1020
[8]Cooke, J., Sullivan, M., Gal-Yam, A., et al., 2012, Nature, 491, 228
[9]Fruchter, A., Levan, A.J., Strolger, L., et al., 2006, Nature, 441, 463
[10]Fynbo, J.P.U., Gorosabel, J., Smette, A., et al., 2005, ApJ, 633, 317
[11]Fynbo, J.P.U., Prochaska, J.X., Sommer-Larsen, J., et al., 2008, ApJ, 683, 321
[12]Gal-Yam, A., 2012, Science, 337, 927
[13]Heger, A., Fryer, C.L., Woosley, S.E., et al., 2003, ApJ, 591, 288
[14]Hunt, L., Palazzi, E., Rossi, A., et al., 2011, ApJ, 736, L36
[15]Krühler, T., Greiner, J., Schady, P., et al., 2011, A&A, 534, A108
[16]Krühler, T., Fynbo, J.P.U., Geier, S., et al., 2012, A&A, 546, A8
[17]Leitherer, C., Tremonti, C.A., Heckman, T.M., et al., 2011, AJ, 141, 37
[18]Levesque, E., Kewley, L.J., Berger, E., et al., 2010, AJ, 140, 1557
[19] Levesque, E.M., Kewley, L.J., Graham, , et al., 2010, ApJ, 712, L26
[20]Maiolino, R., Nagao, T., Grazian, A., et al., 2008, A&A, 488, 463
[21]Martin, C.L., Shapley, A.E., Coil, A.L., et al., 2012, ApJ, 760, 127
[22]Michałowski, M., Hjorth, J., & Watson, D., 2010, A&A, 514, A67
[23]Michałowski, M.J., Kamble, A., Hjorth, J., et al., 2012, ApJ, 755, 85
[24]Neill, J.D., Sullivan, M., Gal-Yam, A., et al., 2011, ApJ, 727, 15
[25]Niino, Y., Hashimoto, T., Aoki, K., et al., 2012, PASJ, 64, 115
[26]Perley, D.A., Modjaz, M., Morgan, A.N., et al., 2012, ApJ, 758, 122
[27]Pontzen, A., Deason, A., Governato, F., et al., 2010, MNRAS, 402, 1523
[28]Rau, A., Savaglio, S., Krühler, T., et al., 2010, ApJ, 720, 862
[29]Rossi, A., Klose, S., Ferrero, P., et al., 2012, A&A, 545, A77
[30]Salvaterra, R., Maio, U., Ciardi, B., et al., 2013, MNRAS, in press
[31]Savaglio, S., 2012, IAU Symposium, 279, 212
[32]Savaglio, S., Glazebrook, K., Abraham, R.G., et al., 2004, ApJ, 602, 51
[33] Savaglio, S., Glazebrook, K., Le Borgne, D., et al., 2005, ApJ, 635, 260
[34] Savaglio, S., Glazebrook, K., & Le Borgne, D., 2009, ApJ, 691, 182
[35]Savaglio, S., Rau, A., Greiner, J., et al., 2012, MNRAS, 420, 627
[36]Tanvir, N.R., Rol, E., Levan, A.J., et al., 2010, ApJ, 725, 625
[37]Tanvir, N.R., Levan, A.J., Fruchter, A.S., et al., 2012, ApJ, 754, 46
[38]Thöne, C., Campana, S., Lazzati, D., et al., 2011, MNRAS, 414, 479
[39]Vergani, S.D., Piranomonte, S., Petitjean, P., et al., 2011, Astron. Nach., 332, 292

Related content

Powered by UNSILO

The Cosmic Evolution of Gamma-Ray Burst Host Galaxies

  • S. Savaglio (a1)


Full text views

Total number of HTML views: 0
Total number of PDF views: 0 *
Loading metrics...

Abstract views

Total abstract views: 0 *
Loading metrics...

* Views captured on Cambridge Core between <date>. This data will be updated every 24 hours.

Usage data cannot currently be displayed.