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 (1999-2009) 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-SpainORM-Spain

Izaña-SpainIzaña-Spain

SAO-RussiaSAO-Russia

PdB-PdB-FranceFrance

Calar Alto-Calar Alto-SpainSpain

Mt. John-New ZealandMt. John-New ZealandBOOTES-BOOTES-SpainSpain

OSN-OSN-SpainSpain

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 detectedin early afterglow spectra (T - T

0 ≈ 11 hours)

GRB afterglow spectroscopy in early phase allows to study SN explosionphysics near moment of core collapse!

Multi pupil fiber spectrograph

SCORPIO - is a multi-mode focal reducer of the 6-meter telescope (imaging, long-slit andmulti-slit spectroscopy, broad-bandpolarimetry 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 iswell known for SNe(comfirmation of SN-GRB connection)

Nebular phase

Photospheric phase

XRF080109/SN2008D spectral evolution

High-velocity Hα line

The spectra showedpossible high-velocityHα line (more detailsin the other presentation)

GRB090726 early spectroscopy

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

ZOT

= 2.71

SWIFT J195509+261406: candidate to Galactic magnetar

Castro-Tirado et al., 2008, Nature, vol 455, issue 7212, pp 506-509

In initial phase (first 3 days)the object showed burst activityin optics and X-rays.

a) light curve in optics (IC band)b) light curve in X-rays (SWIFT/XRT and XMM-Newton)

Log-normal distribution of optical bursts

SWIFT J195509+261406: candidate to Galactic magnetar

BTA/SCORPIO deep images of SWIFT J195509+261406 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 050709 and 050724 (Hjorth et al. 2005, Berger

et al. 2006). Flaring in GRB 050724

(Barthelmy et al. 2005) not easy to model.

BTA images of GRB 050509b, first short GRB X-ray afterglow localized accurately by Swift (Castro-

Tirado et al. 2005). In an elliptical galaxy at z = 0.225. 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 ourunderstanding 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., with6-meter telescope contribution)!

Spectroscopy of dark GRB051022 host galaxy

Redshift from emission lines z = 0.809

Corrected forinternal extinctionSFR ≈ 50 M

☼/yr

Some applications of GRB host galaxies observations

Deep GRB021004 host galaxy field

Up to 1000 objects in 4.3x4.3arcmin field (in the R-band, withR

lim ≈ 26.5).

Study galaxies at intermediateredshifts 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 4.3x4.3arcmin field (in the R-band, withR

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!