The observations of GRB optical afterglow with 6-meter telescope: recent results and future plans...
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Transcript of The observations of GRB optical afterglow with 6-meter telescope: recent results and future plans...
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!