The observations of GRB optical afterglow with 6-meter telescope: recent results and future plans T.A. Fatkhullin and SAO RAS follow-up team Nizhnij Arkhyz, 2009

History of the 6-meter telescope proposal 10 years ( ) of the GRB observation program (P.I.: A.J. Castro-Tirado) Collaboration with Italy, Spain, USA, France, India, Ukraine, Turkey colleagues (from 0.5 to 8 meter optical and NIR telescopes, IRAM 30-m mm telescope). You are wellcome!

ORM-Spain Izaña-Spain SAO-Russia SAO-Russia PdB- France Calar Alto- Spain Mt. John-New Zealand Mt. John-New Zealand BOOTES- Spain OSN- Spain

2.34m, VBT, Kavalur The “Indian” connection 1.04m, ST, Naini Tal 2.01m, HCT, IAO

Main observational aims: Early spectroscopy (GRB-SN connection, environment) Spectroscopic monitoring (GRB-SN connection, progenitors) Deep early photometry for short-lived GRBs (Progenitors, GRB bimodality) Photometry and spectroscopy of GRB host galaxies (Progenitor environment, hosts properties)

Early spectroscopy of the GRB030329/SN2003dh afterglow SN features was detected in early afterglow spectra (T - T 0 ≈ 11 hours) GRB afterglow spectroscopy in early phase allows to study SN explosion physics near moment of core collapse! Multi pupil fiber spectrograph

SCORPIO - is a multi-mode focal reducer of the 6-meter telescope (imaging, long-slit and multi-slit spectroscopy, broad-band polarimetry and spectropolarimetry) The main instrument used 6-meter telescope instrumentation

Early spectra of the XRF060218/SN2006aj and its spectral evolution Spectral evolution showed a transition from photospheric to nebular phase as it is well known for SNe (comfirmation of SN-GRB connection) Nebular phase Photospheric phase

XRF080109/SN2008D spectral evolution High-velocity Hα line The spectra showed possible high-velocity Hα line (more details in the other presentation)

GRB early spectroscopy GRB afterglow spectroscopy provides detailed analysis of the ISM of actively- starforming galaxies (metallicity, extinction curve, etc). Z OT = 2.71

SWIFT J : candidate to Galactic magnetar Castro-Tirado et al., 2008, Nature, vol 455, issue 7212, pp In initial phase (first 3 days) the object showed burst activity in optics and X-rays. a) light curve in optics ( I C band ) b) light curve in X-rays (SWIFT/XRT and XMM-Newton) Log-normal distribution of optical bursts

SWIFT J : candidate to Galactic magnetar BTA/SCORPIO deep images of SWIFT J field After a 3-day activity the object has disappeared in the deep optic and NIR images

First Detections of optical and radio afterglows for GRB and (Hjorth et al. 2005, Berger et al. 2006). Flaring in GRB (Barthelmy et al. 2005) not easy to model. BTA images of GRB b, first short GRB X- ray afterglow localized accurately by Swift (Castro- Tirado et al. 2005). In an elliptical galaxy at z = Support for binary mergers (Gehrels et al. 2005). Photometry of short-lived GRB050509B

GRB host galaxies observations Hubble diagram for GRB host galaxies (beginning of the program) Host galaxies observations are very important for our understanding of progenitor nature!.... History of heavy elements enrichment, dust obscuration and star-formation history in the Universe Most distant GRB detected so far is 8.3 (Tanvir et al., with 6-meter telescope contribution)!

Spectroscopy of dark GRB host galaxy Redshift from emission lines z = Corrected for internal extinction SFR ≈ 50 M ☼ /yr

Some applications of GRB host galaxies observations Deep GRB host galaxy field Up to 1000 objects in 4.3x4.3 arcmin field (in the R-band, with R lim ≈ 26.5). Study galaxies at intermediate redshifts of 1-3. Estimations show we can detect ~1 CC-SNe per year

«Magnitude-counts» diagram in R-band Some applications of GRB host galaxies observations Up to 1000 objects in 4.3x4.3 arcmin field (in the R-band, with R lim ≈ 26.5).

Future plans Start of SNe observational program: systematic studies of properties of SNe with and without GRB, assymetry of explosion, progenitor circum-stellar enviroment Spectroscopy and deep photometry of afterglow (to be continued) Polarimetry and spectropolarimetry: assymetry of explosion, structure of ejecta New instrumentation: IFU for rapid-response spectroscopy?

Thank you!