Spectral and photometric monitoring of distant SNe

in SAO RAS

A. S. Moskvitin, T. A. Fatkhullin, V. V. Sokolov,

V. N. Komarova, E. Sonbas, R. Roy, et al.

The study of core-collapse supernovae (SNe) is

particularly interesting in general, because it is believed

that long-duration Gamma-Ray Bursts (GRBs) are

connected with SNe. Therefore GRBs can be produced by

core collapse of massive stars. So, the study of GRBs can

be said to constitute a new phase of the study of the

same massive (core-collapse) SNe but from the start of

the event. In such cases spectroscopic and photometric

observations of core-collapse SNe in general are of the

great importance for understanding the mechanism of the

explosion of the massive SN itself, because this explosion

mechanism of most massive progenitors is still a puzzle.

Main goals of observational program

Early observations of recently discovered core-collapse SNe (shock break-out effect, and GRB-SN connections).

Nebular phase observations of core-collapse SNe (axially-symmetrical explosion).

The 6-meter telescope as a part of the international monitoring of SNe

participiants of the program:

SAO RASVladimir V. SokolovTimur A. FatkhullinViktoria N. KomarovaAlexander S. MoskvitinTatiana N. SokolovaGrigorii M. BeskinVladimir L. PlokhotnichenkoSergei V. KarpovVitaly P. GoranskijValerii V. VlasyukOlga I. SpiridonovaAzamat F. ValeevAleksandr N. Burenkov

SAI MSU (GAISH)Dmitry Yu. TsvetkovIgor' M. Volkov

Turkey

Eda Sonbas (University of Cukurova)

Aysun Akyuz (University of Cukurova)

Spain

Alberto Javier Castro-Tirado (IAA –

CSIC, Granada)

Javier Gorosabel (IAA – CSIC, Granada)

India

Shashi Bhushan Pandey (ARIES)

Brajesh Kumar (ARIES)

Rupak Roy (ARIES)

USA

Andrew Drake (California Institute of

Technology)

Italy

Cosimo Inserra (INAF)

Stefano Benetti (INAF)

Observations with BTA and Zeiss-1000, +…February, 24, 27 observations with the

Zeiss-1000:1) SN 2009M2) SN 2009Z3) CSS090213_083642+0914054) CSS090219_095526-0128215) CSS090214_102503+1758216) CSS090216_100910+075434 =

2009bx (published in CBET#1744)

March, 05 observations with the Zeiss-1000:

7) SN 2009af8) SN 2009ao

March,26 - April,4 observations with the Zeiss-1000:

9) SN 2009bw (future publication with S.Benetti, C.Inserra, D.Y. Tsvetkov, I.M.Volkov)

10) CSS090319:094627-13080611) SN 2009ba

12) SN 2009az13) CSS090319:125916+271641

= 2009cb (published in CBET#1752)

14) CSS090317:140750+363837 15) CSS090319:142155+260102

= 2009db (published in CBET#1760)

16) CSS090319:152356-08191817) SN 2009ay (future

publication with D.Y. Tsvetkov, I.M.Volkov)

18) SN 2008gz (future publication with R. Roy)

19) SN 2008in (future publication with R. Roy)

20) SN 2009bz

April, 3 observations with the BTA:

SN 2009bw

SN 2009az

SN 2008gz

SN 2008in

CSS090317:140750+363837

CSS090319:142155+260102

Observations with BTA and Zeiss-1000 (2)

April, 23-26 observations with the

BTA:

SN 2008in

21) CSS090421:133609+340319

(published in CBET#1791)

22) SN 2009de (our future publication

with A. Drake)

23) SN 2009dm (only R-band

photometry)

24) CSS090422:150104+431314

(published in CBET#1791)

25) CSS080928:160837+041627

(future publication with A. Drake) = SN

2008iy

May, 11, 12, 29; Jyly, 23, 24

monitoring of SN 2009de with the

Zeiss-1000

May, 14-18 observations with the BTA:

SN 2009de

CSS090514:150635+215115

26) CSS090516:163900+175858 (published in

CBET#1801)

Spectral monitoring of SN 2008iy with the

BTA:

Jun, 20/21; Jyl, 25/26, Jyl, 26/27; Sep, 25/26.

Monitoring of SN 2009bw with the Zeiss-

1000:

Aug, 24/25; Sep. 18/19

Monitoring of SN 2009ay with the Zeiss-1000:

Jun. 27/28; Jun. 28,29; Jul. 25/26; Aug. 01/02;

Aug 15/16; Aug24/25; Sep. 17/18

Shematic model of asymmetric explosion of a GRB/SN progenitor

…a strongly non-spherical explosion may be a generic feature of core-collapse supernovae of all types.

…Though while it is not clear that the same mechanism that generates the GRB is also responsible for exploding the star.

astro-ph/0603297

Leonard, Filippenko et al.

Though the phenomenon (GRB) is unusual, but the object-source (SN) is not too unique.The closer a GRB is, the more features of a SN.

The shock breaks out through the wind

The windenvelopeof size ~1013 cm

56Ni synthesizedbehind the shock wave

SNe are the most violent explosions at the end of the star's life.

SNe are classified according to their spectra and light curve.

The core-collapse of massive supernovae

SNe spectra and classification

arXiv 0706.1086 Turatto, S. Benetti, A. Pastorello

The light curves showed non-monotonic behaviour with two maxima. (The same first maximum was observed in SN1987A and SN1993J and attributed to shock break-out.)

SN 2006aj, UBVRIJ light curves (Sonbas et al., arXiv:0805.2657)

the end of the shock break-out phase

The earlest spectrum of SN 2006aj (BTA)

Δt=2.55d, Vphot=VmineHI

=33,000 km/s; Tbb

=9,000K

The general belief is that core collapse supernovae connected with XRF/GRBs event can be

naturally explained by the aspherical axially-symmetrical explosion of massive SNe. The

common assumption is that in the case of an XRF type flash the observer is located outside

the cone where for some reasons the bulk of gamma-ray radiation is concentrated. The

asphericity is generally observed in the nebular phase observations.

We can not see any GRB event

connected with SN2003jd

Thus, the doubled peaked [OI] emission

must be observed for SNe which were

not accompanied with GRBs, like

SN2008D. And the single peak of [OI]

emission is observed in the nebular

phase of SNe which are accompanied

with GRBs, as in the case of

GRB060218/SN2006aj.

Nebular phase

Nebular spectra of SN 2006aj and SN 2008D

VLT, September, 19/20, 2006Mazzali et al., 2007 ApJ 661, 892

BTA, August, 27, 2006

[OI]6300A in nebular phase of Ib-c type SN 2008D, Modjaz et al. (arXiv:0805.2201)

SN 2006ajSN 2006aj

SN 2008D

Main goals of observational program

Early observations of recently discovered core-collapse SNe (shock break-out effect, and GRB-SN connections).

Nebular phase observations of core-collapse SNe (axially-symmetrical explosion).

Telescopes & programs in SAO

Proposals (SN+GRB programs): 8 nights (4 fixed + 4 ToO) of 1st semester of 2009 year

telescopes/devices:BTA/Scorpio (photometry and long-slit spectroscopy modes)

BTA/MANIA (photometry, polarimetry and spectroscopy with R=100)

Zeiss-1000 + other I

+ other telescopes I:international program

1.04 m Sampurnanand Telescope, India (R. Roy)2-m IUCAA Telescope, Pune, India (R. Roy)2-m Zeiss, Terskol peak, (I. Sokolov & Co)0.7m AZT-2, SAI MSU (D. Yu. Tsvetkov)0.5m telescope, State Astronomical Observatory,

Slovakia (I. M. Volkov)CSS telescopes: 0.68m, 0.5m, 1.5m (A. Drake)+ other II (Italy)

+ other telescopes II:Italy part of collaboration

TNG - Telescopio Nazionale Galileo, 3.58m optical/infrared telescope; Island of San Miguel de La Palma

Calar Alto - (3.5m or 2.2m or 1.23m) The German-Spanish Astronomical Center at Calar Alto is located in the Sierra de Los Filabres (Andalucia, Southern Spain) north of Almeria.

NOT - Nordic Optical Telescope, 2.6-m, Observatorio del Roque de los Muchachos, island of La Palma in the Canaries

Ekar - 1.82m (Cima Ekar-Asiago, Italy) LT - Liverpool 2.0-m fully robotic telescope Pennar 1.22m - Astrophysical Observatory, Asiago, Italy

Catalina Real-time Transient Survey

arXiv: 0809.1394

transient events (SNe, hazard asteroids, CV, AGN, etc.), timescales: seconds – years, ~ few 10000 sq degrees (~1200 sq. degrees per night), -30 < Decl. < 70 3 identical system of registration:

1) original Catalina Sky Survey (CSS), 68 cm (27 inch) f/1.9 Schmidt

telescope near Mt. Bigelow (FOV ~ 9 degrees);

2) Siding Springs Survey (SSS), 0.5 meter (20 inch) Uppsala Schimidt

telescope (FOV ~ 4.2 degrees);

3) Mt. Lemmon Survey (MLSS), 1.5 meter (60 inch) f/2 telescope (FOV ~

1 degree).

CCD 4096x4096 (Thermo-electrical cooling ~ -100C), dark ~ 1 e- /hour. 4 x 30 sec. exposures with 30 min spacing, limit magnitude V = 21.5 (30 sec., 1.5-m telescope)

http://www.lpl.arizona.edu/css/css_facilities.html

arXiv:0810.4527v1

arXiv:0802.3465v1

arXiv:0802.3465v1

List of newly discovered objects

Statistics of 2008 year (objects up to 18m and Decl.>18°): almost half – core collapse SNe.(Data from www.cfa.harvard.edu/iau/lists/RecentSupernovae.html)

CSS http://nesssi.cacr.caltech.edu/catalina/AllSN.htmlCBET http://www.cfa.harvard.edu/iau/cbet/RecentCBETs.html, ATEL http://www.astronomerstelegram.org/and in the siteshttp://astrosurf.com/snweb2/2009/SN2009Full.htmhttp://www.supernovae.net/

GRB 021004 host galaxy field GRB 021004 host galaxy: deep field of size 4.05΄×4.05΄

Data reduction processing includes the primary reduction of direct images, selection of faint

galaxies in images, photometry in four filters (B,V,R,I), estimation of galaxy angular size and photometric red-shift, the construction of relation between different observed values.

183 objects with S/N>3 in BVRI-bands

limit stellar magnitudes for 183 objects: 26.0 (B) during 3600s, 25.5 (V) during 3600s,

25.0 (R) during 2700s, 24.5 (I) during 1800s.

Fig.10. Differential counts of galaxies in the V filter.

Galaxies in the field of GRB 021004

FOV 4’.3 x 4’.3: ~1 СС-SNe per

year

or

~ 500 SNe up to ~25m per hour at ½ of sky

(without corrections of host extinction)

Fig.12. Distribution of galaxies in the field of GRB 021004 by photometric red shifts.

Some results of observations(one night as exampe):

March-April'09 observations in SAOAvailable interesting objects for observations with the BTA and Zeiss-1000

List of nebular phase supernovae

SNe in nebular phase for spectroscopy of [OI] 6300,6363AA: SNe of end 2008 – begin 2009SN 2008in (II-P)SN 2008gz (II)

Obtained spectra (April, 3/4) SN 2009bw (4 x 300 sec) SN 2009az (2 x 600 sec + 2 x 900 sec.) SN 2008gz (3 x 900 sec.) SN 2008in (2 x 900 sec.) CSS 090317a (2 x 600 sec.) CSS 090319c (2 x 600 sec.)

SuperNova IDentification code

ApJ, 666, 1024, (2007); arXiv:0709.4488

SNID and CSS 090319c (z=0.078)

CSS 09019cZeiss-1000 (SAO RAS) field

http://nesssi.cacr.caltech.edu/catalina/20090319/903191260704110940p.html

090317a and 090319c

z=0.03 (CBET#1747), Ia type

CSS 090317aZeiss-1000 (SAO RAS) field

http://nesssi.cacr.caltech.edu/catalina/20090317/903171350634142473p.html

SN 2008bw & SN 2009az

Zeiss-1000 (SAO RAS) fields

SN 2008gz & SN 2008in: nebular phase

Zeiss-1000 (SAO RAS) fields

SN 2008gz: report of

Rupak Roy

Another interesting objects:

SN 2009de: z=0.3, M~-21.8, type Ic-pec SN

SN 2009de: line identification, redshift

CSS080928:160837+041627 = SN 2008iy

five BTA spectra: Apr, 23/24; Jun, 20/21; Jyl, 25/26, Jyl, 26/27; Sep, 25/26QSO or SN type IIn (narrow lines)plato at lightcurve

Publications: Discovering of SN 2009bx (CSS090216:100910+075434), B, V, Rc photometry with the Zeiss-1000 are published in

CBET #1744. (Drake, A. J.; Djorgovski, S. G.; Williams, R.; Mahabal, A.; Graham, M. J.; Catelan, M.; Beshore, E. C.; Larson, S. M.; Hill, R.; Christensen, E.; Moskvitin, A., «Supernova 2009bx», 2009)

SN 2009cb (CSS090319:125916+271641), Rc photometry with the Zeiss-1000: CBET # 1752 (Drake, A. J.; Mahabal, A.; Djorgovski, S. G.; Williams, R.; Graham, M. J.; Hsiao, E. Y.; Graham, M. L.; Pritchet, C. J.; Balam, D.; Moskvitin, A.; Catelan, M.; Beshore, E. C.; Larson, S. M.; Christensen, E., «Supernova 2009cb», 2009)

SN 2009db (CSS090319:142155+260102), Rc photometry (Zeiss-1000), results of spectroscopy(BTA+Scorpio):

CBET #1760 (Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Williams, R.; Graham, M. J.; Moskvitin, A. S.; Fatkhullin, T.

A.; Sokolov, V. V.; Spiridonova, O. I.; Valeev, A. F.; Sonbas, E.; Pandey, S. B.; Kumar, B.; Roy, R.; Tsvetkov, D. Y.;

Catelan, M.; Beshore, E. C.; Larson, S. M.; Christensen, E., «Supernova 2009db», 2009)

SN 2009dy & SN 2009dw ( CSS090422:150104+431314 & CSS090421:133609+340319), SNID comparison with the

BTA+Scorpio spectra, redshift estimates: CBET #1791 (Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Williams, R.;

Graham, M. J.; Moskvitin, A. S.; Fatkhullin, T. A.; Sokolov, V. V.; Spiridonova, O. I.; Valeev, A. F.; Sonbas, E.; Pandey,

S. B.; Kumar, B.; Roy, R.; Tsvetkov, D. Y.; Catelan, M.; Beshore, E. C.; Larson, S. M.; Christensen, E., «Supernovae

2009du-2009dy», 2009)

SN 2009ew (CSS090516:163900+175858) SNID comparison with the BTA+Scorpio spectrum, redshift estimations:

CBET # 1815 (Drake, A. J.; Williams, R.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Fatkhullin, T. A.; Moskvitin, A.

S.; Sokolov, V. V.; Spiridonova, O. I.; Valeev, A. F.; Sonbas, E.; Pandey, S. B.; Kumar, B.; Roy, R.; Tsvetkov, D. Y.;

Balam, D.; Catelan, M.; Beshore, E. C.; Larson, S. M.; Christensen, E., «Supernova 2009ew», 2009)

+ few conference reports

Publications in progress: SN 2008gz (II type) - SYNOW interpretation of all spectra (BTA+Scorpio,

TNG+DOLORES (Italy), IGO+IFOSC (India)): lines identification,

expansion velocities, chemical composition. Multicolour lightcurve (104 cm

Sampurnanand Telescope (India), BTA): distance, evolution, luminocity,

etc. (Rupak Roy, Brajesh Kumar, Shashi B. Pandey (ARIES, India),

Stefano Benetti (INAF - OAPd, Italy) и Eda Sonbas (University of

Cukurova, Turkey)).

SN 2008in (II type) – SYNOW interpretation of all spectra, multicolor

lightcurve (international monitoring with the BTA, Zeiss-1000, TNG, REM,

Pennar 1.22m, Calar Alto, NOT, NTT), estimation of physical parameters,

comparison with idenical events. (Rupak Roy, Brajesh Kumar, Shashi B.

Pandey (ARIES, India), Stefano Benetti et al. (INAF - OAPd, Italy)).

SN 2009bw (II type): BTA, Zeiss-1000, Calar Alto, NOT, TNG , SWIFT, Ekar 1.82m, LT, 0.7m AZT-2 (SAI MSU, Moscow), 0.5m (Slowakia), (Stefano Benetti, Cosimo Inserra (INAF - OAPd, Italy), D. Yu. Tsvetkov, I. M. Volkov (SAI MSU))

SN 2009de (Ic pec, z=0.31): SYNOW, RV-lightcurves (BTA, Zeiss-

1000, CSS, Palomar 200), Andrew Drake (California Institute of

Technology, USA)

SN 2009ay (II): Photometry with Zeiss-1000, 0.7m AZT-2 (SAI MSU,

Moscow), 0.5m (Slowakia), (D. Yu. Tsvetkov, I. M. Volkov (SAI

MSU))

CSS080930:022409+264010 (=SN 2008iy, IIn or QSO): spectra from

BTA and Palomar 200, lightcurve (CSS), nature of source (SAO

team+ Andrew Drake (California Institute of Technology, USA))

Publications in progress:

Thank You

light curve of SN 1987Athe shock break-outphase

Imshennik & Nadyozhiin, UFN, 156, 261, (1988), fig.16