Local Universe Local Universe Supernovae and Their Supernovae and Their

Host GalaxiesHost Galaxies

Artashes PetrosianArtashes PetrosianByurakan Observatory, ArmeniaByurakan Observatory, Armenia

The TeamThe TeamByurakan Observatory (Armenia): A. HakobyanByurakan Observatory (Armenia): A. Hakobyan

Catania Observatory (Italy): M. TurattoCatania Observatory (Italy): M. TurattoCNR-IRA (Italy): F. MannucciCNR-IRA (Italy): F. Mannucci

IAP (Paris, France): D. Kunth, G. MamonIAP (Paris, France): D. Kunth, G. MamonINAF-OAC (Italy): M. Della ValleINAF-OAC (Italy): M. Della Valle

Padova Observatory (Italy): E. Cappellaro, H. Navasardyan, Padova Observatory (Italy): E. Cappellaro, H. Navasardyan, STScI: R. Allen, C. Leitherer, J. MacKenty, B. McLean, STScI: R. Allen, C. Leitherer, J. MacKenty, B. McLean,

N. PanagiaN. Panagia

Historical Milky Way Historical Milky Way SupernovaeSupernovae

• The earliest recorded The earliest recorded SN185 in 185AD.SN185 in 185AD.

• The Crab Nebula The Crab Nebula associated with the associated with the

1054 supernova 1054 supernova

• Tyco’s Nova SN1572Tyco’s Nova SN1572

• Kepler's supernova Kepler's supernova Remnant, SN 1604 Remnant, SN 1604

• G1.9+0.3: Youngest G1.9+0.3: Youngest (~140 yr) known SN(~140 yr) known SN

Extragalactic Supernovae Extragalactic Supernovae SN 1998SSN 1998S

• First extragalactic SNe (S First extragalactic SNe (S Andromedae) was discovered Andromedae) was discovered in Andromeda galaxy in in Andromeda galaxy in 1885. 1885.

• In 1934 Baade & Zwicky In 1934 Baade & Zwicky (1934) define supernovae as (1934) define supernovae as separate class of objects. separate class of objects.

• First systematic SN search First systematic SN search was initiated by Zwicky in was initiated by Zwicky in 1936. 1936.

• Currently the number of Currently the number of discovered SNe is discovered SNe is approaching to 5000 from approaching to 5000 from which about 50% have been which about 50% have been discovered in 21discovered in 21stst century. century.

Why studying SNeWhy studying SNePhysics of the explosion:Physics of the explosion:

• EnergeticsEnergetics

• NucleosynthesisNucleosynthesis

• Compact remnantsCompact remnants

• ……SNe as tools:SNe as tools:

• Distance indicatorsDistance indicators

• Probes of (late) evolution of stars and progenitors Probes of (late) evolution of stars and progenitors systems (mass loss, …)systems (mass loss, …)

• Probes of extinction in external galaxiesProbes of extinction in external galaxies

• Probes of Star Formation HistoryProbes of Star Formation History

• ……

Taxonomy 2003Taxonomy 2003Turatto 2003

Classification of SupernovaeClassification of SupernovaeTuratto 2003Turatto 2003

Light curves are homogeneous (!)

SNIa: Light curvesSNIa: Light curves

1994D 1996X 1992A

Spectra are homogeneous

Summary of SNIaSummary of SNIa

Observational properties:

•fairly homogeneous

• MB≈MV=-19.5

• show O,Mg,S,Si,Ca near maximum, Fe at late phases

• no hydrogen

• no radio or X-ray emission

• occur in all type of galaxies (E included)

• in spirals, not strongly associated with HII regions

Interpretation: Thermonuclear disruption of CO WDs which Thermonuclear disruption of CO WDs which accreted their mass up to the Chandrasekhar limit via mass accreted their mass up to the Chandrasekhar limit via mass transfer from a companion in binary systems.transfer from a companion in binary systems.

SN II: Light curvesSN II: Light curves

Patat et al. 1994

SNII: Spectral varietySNII: Spectral variety

IIP

IIL

IIn

IIpec

IIb

1987A

1980K

1988Z

1997cy

1993J

56Ni56Co56Fe

SN Ib/c: Light curvesSN Ib/c: Light curvesElmhamdi et al. 2004

type II type Ib

SN 1993JSN 1993JBarbon et al. 1995

Summary of CC SNeSummary of CC SNe

Observational properties

•NOT homogeneous

• show H, He, O, Ca …...

• from small to huge radio and X-ray emission

• occur only (!!) in spiral galaxies and are associated with star forming regions

• leave collapsed remnant (NS or BH) [Crab]

• emit neutrinos and gravitational waves

InterpretationInterpretation: : The core collapse in The core collapse in massive stars (massive stars (MM≥8≥8MM) at the end of a series ) at the end of a series

central nuclear burnings which end up with the central nuclear burnings which end up with the formation of an iron core.formation of an iron core.

• variable envelope size and mass

• variable 56Ni mass

• variable CSM density and distribution

SN classification IISN classification II

Fields of study of SNe and their host galaxiesFields of study of SNe and their host galaxies

• SNe in isolated galaxies, in pairs and in groups of galaxies SNe in isolated galaxies, in pairs and in groups of galaxies (Petrosian & Turatto 1995, Navasardyan et al. 2001)(Petrosian & Turatto 1995, Navasardyan et al. 2001)

• SNe in active and star forming galaxies (Turatto et al. 1989, SNe in active and star forming galaxies (Turatto et al. 1989, Petrosian & Turatto 1990, 1992, Petrosian et al. 2005, Hakobyan Petrosian & Turatto 1990, 1992, Petrosian et al. 2005, Hakobyan 2008)2008)

• Radial distribution of CC SNe in spiral galaxies (Hakobyan et al. Radial distribution of CC SNe in spiral galaxies (Hakobyan et al. 2008a)2008a)

• Early type galaxies with CC SNe (Hakobyan et al. 2008b)Early type galaxies with CC SNe (Hakobyan et al. 2008b)

SNe in isolated galaxies, in pairs and in groups of SNe in isolated galaxies, in pairs and in groups of galaxies. Navasardyan et al. (2001)galaxies. Navasardyan et al. (2001)

• The aim: To investigate : To investigate the influence of the influence of environment on SN environment on SN production.production.

• 22 SNe in 18 isolated 22 SNe in 18 isolated galaxiesgalaxies

• 48 SNe in 40 galaxies 48 SNe in 40 galaxies members of 37 pairsmembers of 37 pairs

• 211 SNe in 170 galaxies 211 SNe in 170 galaxies members of 116 groupsmembers of 116 groups..

SNe in isolated galaxies, in pairs and in groups of galaxiesSNe in isolated galaxies, in pairs and in groups of galaxies

ConclusionsConclusions::• Radial distributions of CC SNe in galaxies located in different Radial distributions of CC SNe in galaxies located in different

environments are similar.environments are similar.• SNe discovered in pairs show isotropic azimuthal distributions and SNe discovered in pairs show isotropic azimuthal distributions and

do not favor a particular direction with respect to the companion do not favor a particular direction with respect to the companion galaxy.galaxy.

• SN rate in galaxies members of pairs is > 40% higher than in SN rate in galaxies members of pairs is > 40% higher than in average galaxy and > 60% higher than in members of groups.average galaxy and > 60% higher than in members of groups.

• With the possible exception of strongly interacting systems the With the possible exception of strongly interacting systems the host environment has no influence of SN production.host environment has no influence of SN production.

SNe in active and star forming (A/SF) galaxies.SNe in active and star forming (A/SF) galaxies.List of the problems addressedList of the problems addressed

• To what extent does the nuclear A/SF affect the host.To what extent does the nuclear A/SF affect the host.

• To determine the rates of SNe in A/SF and normal galaxies.To determine the rates of SNe in A/SF and normal galaxies.

• To compare integral properties (morphology, luminosity etc.) of the To compare integral properties (morphology, luminosity etc.) of the hosts of SNe.hosts of SNe.

• To determine the radial distribution of SNe in spiral galaxies.To determine the radial distribution of SNe in spiral galaxies.

• To determine SNe and spiral arms connection.To determine SNe and spiral arms connection.

• To study association of SNe with SF regions.To study association of SNe with SF regions.

The samples of galaxies for SNe The samples of galaxies for SNe searchsearch

• Markarian galaxies (Petrosian et al. 2007) 1544Markarian galaxies (Petrosian et al. 2007) 1544

• Second Byurakan Survey galaxies 1401Second Byurakan Survey galaxies 1401

• NGP +30NGP +30o o zone A/SF galaxies (Petrosian et al. 2008) zone A/SF galaxies (Petrosian et al. 2008) 303303

• NGP +30NGP +30oo zone Normal galaxies (Petrosian et al. 2008) zone Normal galaxies (Petrosian et al. 2008) 878878

Discovered SNeDiscovered SNe

• In Markarian galaxies 47 SNe in 41 galaxiesIn Markarian galaxies 47 SNe in 41 galaxies

• SBS galaxies 10 SNe in 6 galaxies (5 Mrks)SBS galaxies 10 SNe in 6 galaxies (5 Mrks)

• A/SF NGP galaxies 26 SNe in 23 galaxiesA/SF NGP galaxies 26 SNe in 23 galaxies

• Normal NGP galaxies 32 SNe in 29 galaxiesNormal NGP galaxies 32 SNe in 29 galaxies

The rate of SNe in A/SF and Normal galaxies. The rate of SNe in A/SF and Normal galaxies. Previous resultsPrevious results

• The rate of SNe in Markarian galaxies does not differ from the The rate of SNe in Markarian galaxies does not differ from the corresponding value of normal galaxies (Turatto et al. 1989). corresponding value of normal galaxies (Turatto et al. 1989).

• The rate of SNe in the hosts of AGNs does not differ from the The rate of SNe in the hosts of AGNs does not differ from the corresponding value of normal galaxies (Petrosian & Turatto corresponding value of normal galaxies (Petrosian & Turatto 1992).1992).

• The rates of SNe Ia, II and Ib/c in SB galaxies are similar to those The rates of SNe Ia, II and Ib/c in SB galaxies are similar to those measured in normal galaxies (Richmond et al. 1998).measured in normal galaxies (Richmond et al. 1998).

• SNe rates in the hosts of AGNs are not enhanced (Cappellaro et SNe rates in the hosts of AGNs are not enhanced (Cappellaro et al. 1999).al. 1999).

• The rate of SNe Ia is increasing toward galaxies with higher The rate of SNe Ia is increasing toward galaxies with higher activity of star formation (Mannucci et al. 2003).activity of star formation (Mannucci et al. 2003).

The rate of SNe in A/SF and Normal galaxiesThe rate of SNe in A/SF and Normal galaxiesPetrosian et al. (2005)Petrosian et al. (2005)

Frequency per luminosity unit (Frequency per luminosity unit (SNuSNu))aa with standard errors: with standard errors:

____________________________________________________________________________________________________________________________________

Mrk A/SF Normal Cappellaro et al. (1999) Mrk A/SF Normal Cappellaro et al. (1999)

____________________________________________________________________________________________________________________________________

Ntot 316 483 354 9246Ntot 316 483 354 9246

Ia 0.47±0.23(4) 0.33±0.15(4.6) 0.49±0.16(9) 0.20±0.06(69.6) Ia 0.47±0.23(4) 0.33±0.15(4.6) 0.49±0.16(9) 0.20±0.06(69.6)

II+Ib/c 0.85±0.60(2) 0.67±0.36(3.4) < 0.15(0) 0.48±0.19(67.4)II+Ib/c 0.85±0.60(2) 0.67±0.36(3.4) < 0.15(0) 0.48±0.19(67.4)

All 1.32±0.64(6) 1.00±0.39(8) 0.49±0.16(9) 0.68±0.20(137)All 1.32±0.64(6) 1.00±0.39(8) 0.49±0.16(9) 0.68±0.20(137)

____________________________________________________________________________________________________________________________________

a 1SNu = 1SN(100Yr) -1 (1010Lo(B)) -1

The rate of SNe in A/SF and Normal galaxies. The rate of SNe in A/SF and Normal galaxies. ConclusionsConclusions

• The rates of SN Ia and CC SN in A/SF The rates of SN Ia and CC SN in A/SF galaxies are higher than in the galaxies of the galaxies are higher than in the galaxies of the control sample.control sample.

• The rate of CC SN in A/SF galaxies is higher The rate of CC SN in A/SF galaxies is higher than in normal galaxies.than in normal galaxies.

Morphologies of SNe hostsMorphologies of SNe hosts

Mean values:Mean values:

SNIa – 2.5SNIa – 2.5±2.1(28)±2.1(28)

SNII+Ib/c – 4.2±2.5(32)SNII+Ib/c – 4.2±2.5(32)

K-S Probability ofK-S Probability of

Morphology Distribution Morphology Distribution

(distributions are the(distributions are the

same) : - 12%same) : - 12%

0

2

4

6

8

10

12

-2 -1 0 1 2 3 4 5 6 7 8 9 10

Morphology

N

SNe Ia

SNe HII+Ib/c

Morphologies of SNe hosts. Morphologies of SNe hosts. ConclusionsConclusions

• SNe Ia have been discovered in all SNe Ia have been discovered in all galaxy types.galaxy types.

• CC SNe are discovered only in spiral CC SNe are discovered only in spiral and irregular galaxies.and irregular galaxies.

Radial distribution of SNeRadial distribution of SNePrevious resultsPrevious results

• The radial distributions of SNe Ia and SNe II are similar (Bartunov et The radial distributions of SNe Ia and SNe II are similar (Bartunov et al. 1992).al. 1992).

• SNe Ia are more centrally concentrated than SNe II (Howell & SNe Ia are more centrally concentrated than SNe II (Howell & Wheeler 1999 ).Wheeler 1999 ).

• The radial distribution of SNe Ia is in general different from those of The radial distribution of SNe Ia is in general different from those of CC SNe (Wang et al. 1997):CC SNe (Wang et al. 1997):

There is no indication that SNe Ia are more centrally distributed than SNe II.There is no indication that SNe Ia are more centrally distributed than SNe II. There is a relative excess of SNe II compared to SNe Ia near the very center. There is a relative excess of SNe II compared to SNe Ia near the very center. SNe Ib/c are more centrally concentrated than SNe Ia and probably SNe II.SNe Ib/c are more centrally concentrated than SNe Ia and probably SNe II.

• SNe Ib/c may be more centrally concentrated than SNe II (van den SNe Ib/c may be more centrally concentrated than SNe II (van den Bergh 1997).Bergh 1997).

Radial distribution of SNeRadial distribution of SNe

Mean values:Mean values:SNIa – 0.49SNIa – 0.49±0.26(24)±0.26(24)SNII – 0.59±0.31(22)SNII – 0.59±0.31(22)SNIb/c – 0.31SNIb/c – 0.31±0.18(10±0.18(10))

K-S Probability ofK-S Probability ofRadial DistributionRadial Distribution(distributions are (distributions are the same) :the same) :SNe Ia/II - 20%SNe Ia/II - 20%

0

1

2

3

4

5

6

7

8

0.20 0.40 0.60 0.80 1.00 1.20 1.40

[R(SN)/R(25)]corr

N

SNe II

SNe Ib/c

SNe Ia

Radial distribution of SNe. Radial distribution of SNe. ConclusionsConclusions

• The radial distribution of SNe Ia is in general different The radial distribution of SNe Ia is in general different from those of CC SNe.from those of CC SNe.

• There is a relative excess of SNe II compared to SNe Ia There is a relative excess of SNe II compared to SNe Ia events near the very center of the galaxy.events near the very center of the galaxy.

• SNe Ib/c are more centrally concentrated than SNe Ia.SNe Ib/c are more centrally concentrated than SNe Ia.

• SNe Ib/c are more centrally concentrated than SNe II.SNe Ib/c are more centrally concentrated than SNe II.

Distribution of SNe relative to spiral arms and HII Distribution of SNe relative to spiral arms and HII regions. Previous resultsregions. Previous results

• SNe of all types are concentrated towards spiral arms SNe of all types are concentrated towards spiral arms (Bartunov et al. 1994).(Bartunov et al. 1994).

• CC SNe are tightly concentrated in spiral arms; SNe Ia CC SNe are tightly concentrated in spiral arms; SNe Ia show looser concentration (Maza & van den Bergh show looser concentration (Maza & van den Bergh 1996).1996).

• SNe Ia are not correlated with the HII regions (Bartunov SNe Ia are not correlated with the HII regions (Bartunov et al. 1994).et al. 1994).

• SNe II and Ib/c show strong and not significantly SNe II and Ib/c show strong and not significantly different association with HII regions (e.g. Van Dyk et different association with HII regions (e.g. Van Dyk et

al. 1996).al. 1996).

Distribution of SNe relative to spiral arms and Distribution of SNe relative to spiral arms and HII regions. ConclusionsHII regions. Conclusions

• 39% of SNe Ia and 72% of CC SNe are concentrated to 39% of SNe Ia and 72% of CC SNe are concentrated to the spiral arms. the spiral arms.

• There is no SNe Ia associated with HII region.There is no SNe Ia associated with HII region.

• 68% of CC SNe are associated with the HII regions 68% of CC SNe are associated with the HII regions

((71% Van Dyk et al. 199671% Van Dyk et al. 1996))..

• 20% of CC SNe 20% of CC SNe are close to the nuclear regions (< 0.17).

Multivariate Factor Analysis (MFA)Multivariate Factor Analysis (MFA)

• SNe total sample N = 59SNe total sample N = 59

• SNe Ia sample N= 22SNe Ia sample N= 22

• CC SNe N = 32CC SNe N = 32

• Parameters in use:Parameters in use:Morph, AL, M(B), R(Kpc), Inc, R(SN)/R(25), SN type Morph, AL, M(B), R(Kpc), Inc, R(SN)/R(25), SN type

Multivariate Factor Analysis (MFA). Multivariate Factor Analysis (MFA). ConclusionsConclusions

• SNe Ib/c more prefer to be discovered in A/SF hosts than SNe Ib/c more prefer to be discovered in A/SF hosts than SNe II and significantly more than SNe Ia.SNe II and significantly more than SNe Ia.

• SNe II are found preferentially in barred galaxies.SNe II are found preferentially in barred galaxies.

• SNe Ia are closer to the nuclei of A/SF galaxies than to SNe Ia are closer to the nuclei of A/SF galaxies than to the nuclei of normal galaxiesthe nuclei of normal galaxies!!!!!!!!!!

• Closest to the nuclei of the hosts are Ib/c type SNe.Closest to the nuclei of the hosts are Ib/c type SNe.

ASC: CC SNe and their host galaxies.ASC: CC SNe and their host galaxies.Hakobyan (2008)Hakobyan (2008)

• The aimThe aim: Correlation between CC SNe properties and : Correlation between CC SNe properties and integral parameters of their hosts.integral parameters of their hosts.

• The ASC sampleThe ASC sample: 271 SNe (203 SNe II & 68 SNe : 271 SNe (203 SNe II & 68 SNe Ib/c) in 243 hosts.Ib/c) in 243 hosts.

• The methodThe method: MFA with parameters – Morph, Bar, : MFA with parameters – Morph, Bar, AL, M(B), R(Kpc), Inc, SN type & R(SN)/R(25). AL, M(B), R(Kpc), Inc, SN type & R(SN)/R(25).

ASC: CC SNe and their host galaxiesASC: CC SNe and their host galaxies

ConclusionsConclusions::– SNe Ib/c are more SNe Ib/c are more

centrally centrally concentrated than concentrated than SNe II.SNe II.

– CC SNe in A/SF hosts CC SNe in A/SF hosts are more centrally are more centrally concentrated than in concentrated than in normal hosts.normal hosts.

– Latter effect is Latter effect is stronger for SNe stronger for SNe Ib/c.Ib/c.

The radial distribution of CC SNe in The radial distribution of CC SNe in spiral hostsspiral hosts

Hakobyan et al. (2008a)Hakobyan et al. (2008a)

• The aimThe aim: Comparative study of relative : Comparative study of relative radial distribution of CC SNe in spiral radial distribution of CC SNe in spiral galaxies with the distribution of stars and galaxies with the distribution of stars and ionized gas in spiral disks.ionized gas in spiral disks.

• The ASC sampleThe ASC sample: 219 CC SNe (160 SNe II : 219 CC SNe (160 SNe II and 59 SN Ib/c) in 198 spiral hosts (I < and 59 SN Ib/c) in 198 spiral hosts (I < 50°50°;

v< 10000 km sv< 10000 km s-1)..

The radial distribution of CC SNe in host spiral The radial distribution of CC SNe in host spiral galaxiesgalaxies

• ConclusionsConclusions::

– The scale length of CC SNe The scale length of CC SNe distribution is significantly distribution is significantly smaller than that of the stars, smaller than that of the stars, but consistent with that of HII but consistent with that of HII regions.regions.

– SNe Ib/c have significantly SNe Ib/c have significantly smaller scale length than SNe smaller scale length than SNe II.II.

– These tendencies have no These tendencies have no

significant correlations with significant correlations with galaxies integral parameters.galaxies integral parameters.

Summary of conclusions of our studiesSummary of conclusions of our studies

• With the exception of strongly interacting systems the host environment has no influence of With the exception of strongly interacting systems the host environment has no influence of SN production.SN production.

• The rate of CC SN in A/SF galaxies is higher than in normal galaxies.The rate of CC SN in A/SF galaxies is higher than in normal galaxies.

• SNe Ib/c more often discovered in A/SF hosts than SNe II.SNe Ib/c more often discovered in A/SF hosts than SNe II.

• The radial distribution of SNe Ia is different from that of CC SNe.The radial distribution of SNe Ia is different from that of CC SNe.

• SNe Ia are closer to the nuclei of A/SF galaxies than to the nuclei of normal galaxies.SNe Ia are closer to the nuclei of A/SF galaxies than to the nuclei of normal galaxies.

• SNe Ib/c are more centrally concentrated than SNe II.SNe Ib/c are more centrally concentrated than SNe II.

• CC SNe in A/SF hosts are more centrally concentrated than in normal hosts. Latter effect is CC SNe in A/SF hosts are more centrally concentrated than in normal hosts. Latter effect is stronger for SNe Ib/c.stronger for SNe Ib/c.

• Above tendencies have no significant correlations with the integral parameters of host Above tendencies have no significant correlations with the integral parameters of host galaxies.galaxies.

Early type galaxies with CC SNeEarly type galaxies with CC SNeHakobyan et al. (2008b)Hakobyan et al. (2008b)

• Among morphologically Among morphologically classified hosts of CC SNe classified hosts of CC SNe 22 have been classified as 22 have been classified as E or S0 (van den Bergh et E or S0 (van den Bergh et al. 2002, 2003, 2005; al. 2002, 2003, 2005; ASC). ASC).

• Results of our study:Results of our study:

– 17 are misclassified spirals17 are misclassified spirals– 1 is misclassified irregular1 is misclassified irregular– 1 is misclassified ring galaxy1 is misclassified ring galaxy– 2 are mergers2 are mergers– NGC2768 is Elliptical galaxy NGC2768 is Elliptical galaxy

in close interaction. in close interaction.

SN Ia rate calibrated to the unit mass (Mannucci et al. 2005). →

The rate of SN Ia in radio-loud galaxies is ~ 4 times higher than that in radio-quiet galaxies (Della Valle et al. 2005).

SNe Ia are closer to the nuclei of A/SF hosts than to nuclei to normal hosts.

↓

“Prompt” and “Tardy” SNe Ia populations (Mannucci et al. 2006; Greggio et al. 2008).

Projects in ProgressProjects in Progress: Multipurpose study of : Multipurpose study of 3838 galaxies selected from the common southern 3838 galaxies selected from the common southern field of Five SNe, DENIS, 2MASS, POSS-II and SERC field of Five SNe, DENIS, 2MASS, POSS-II and SERC surveyssurveys

• The particular aim of the studyThe particular aim of the study: To determine the rates of : To determine the rates of SN Ia and CC SNe calibrated to the unit mass and stellar SN Ia and CC SNe calibrated to the unit mass and stellar population and relation to integral and nuclear properties of population and relation to integral and nuclear properties of the host galaxies and their local and far environment.the host galaxies and their local and far environment.

• The sampleThe sample: 3838 galaxies in common field of five SNe, : 3838 galaxies in common field of five SNe, DENIS, 2MASS, POSS-II and SERC surveys. Newly DENIS, 2MASS, POSS-II and SERC surveys. Newly determined morphologies and measured optical and near-IR determined morphologies and measured optical and near-IR

parameters.parameters.

Samples in different photometric bandsSamples in different photometric bands

Galaxies Galaxies monitored monitored

SNe SNe discovereddiscovered

In In hosts hosts

UU 10801080 5555 3535

BB 37233723 7373 5252

RR 36973697 7373 5252

II 37023702 7171 5151

JJ 33393339 7373 5252

HH 30983098 7272 5151

KK 32633263 7272 5151

Projects in ProgressProjects in Progress: Multipurpose study of 3838 : Multipurpose study of 3838 galaxies selected from the common southern field of galaxies selected from the common southern field of Five SNe, DENIS, 2MASS, POSS-II and SERC surveysFive SNe, DENIS, 2MASS, POSS-II and SERC surveys

Projects in ProgressProjects in Progress: : SNe in corotation SNe in corotation rings of spiral galaxiesrings of spiral galaxies

NGC4579 (SABb; Sy1.9)NGC4579 (SABb; Sy1.9)• Corotation radius: The radius in Corotation radius: The radius in which angular velocity of which angular velocity of forming spiral arm density wave forming spiral arm density wave and the galactic disk are equal.and the galactic disk are equal.

• Enhanced SF in corotation ring.Enhanced SF in corotation ring. • The aimThe aim: Enhanced SF and : Enhanced SF and

nature of different type of SNe.nature of different type of SNe. • The sampleThe sample: 77 SNe (53 : 77 SNe (53

CCSN; 9 SNIa) in 37 hosts. CCSN; 9 SNIa) in 37 hosts.

Projects in ProgressProjects in Progress: Optical and near-IR surface photometry of : Optical and near-IR surface photometry of SNe environments SNe environments

The motivationsThe motivations::

– Surrounding stellar population can provide information about nature of SNe Surrounding stellar population can provide information about nature of SNe progenitors.progenitors.

– Possible detection of SNe light echoes (Sparks 1994, Boffi et al. 1999).Possible detection of SNe light echoes (Sparks 1994, Boffi et al. 1999).

The sampleThe sample: 158 (v < 10000 km s: 158 (v < 10000 km s-1-1; i < 50°) spiral hosts with 183 SNe (53 SN Ia, 95 SN II, i < 50°) spiral hosts with 183 SNe (53 SN Ia, 95 SN II, 35 SN Ib/c).35 SN Ib/c).

SN1990K (IIP) in NGC150 (vSN1990K (IIP) in NGC150 (vrr = 1584km s = 1584km s-1-1) )