Local Universe Supernovae and Their Host Galaxies Artashes Petrosian Byurakan Observatory, Armenia The Team Byurakan Observatory (Armenia): A. Hakobyan Catania Observatory (Italy): M. Turatto CNR-IRA (Italy): F. Mannucci IAP (Paris, France): D. Kunth, G. Mamon INAF-OAC (Italy): M. Della Valle Padova Observatory (Italy): E. Cappellaro, H. Navasardyan, STScI: R. Allen, C. Leitherer, J. MacKenty, B. McLean, N. Panagia

Historical Milky Way Supernovae The earliest recorded SN185 in 185AD. The earliest recorded SN185 in 185AD. The Crab Nebula associated with the  The Crab Nebula associated with the  1054 supernova 1054 supernova Tyco’s Nova SN1572 Tyco’s Nova SN1572 Kepler's supernova Remnant, SN 1604  Kepler's supernova Remnant, SN 1604  G : Youngest (~140 yr) known SN G : Youngest (~140 yr) known SN

Extragalactic Supernovae SN 1998S First extragalactic SNe (S Andromedae) was discovered in Andromeda galaxy in First extragalactic SNe (S Andromedae) was discovered in Andromeda galaxy in In 1934 Baade & Zwicky (1934) define supernovae as separate class of objects. In 1934 Baade & Zwicky (1934) define supernovae as separate class of objects. First systematic SN search was initiated by Zwicky in First systematic SN search was initiated by Zwicky in Currently the number of discovered SNe is approaching to 5000 from which about 50% have been discovered in 21 st century. Currently the number of discovered SNe is approaching to 5000 from which about 50% have been discovered in 21 st century.

Why studying SNe Physics of the explosion: Energetics Energetics Nucleosynthesis Nucleosynthesis Compact remnants Compact remnants … SNe as tools: Distance indicators Distance indicators Probes of (late) evolution of stars and progenitors systems (mass loss, …) Probes of (late) evolution of stars and progenitors systems (mass loss, …) Probes of extinction in external galaxies Probes of extinction in external galaxies Probes of Star Formation History Probes of Star Formation History …

Taxonomy 2003 Turatto 2003

Classification of Supernovae Turatto 2003

Light curves are homogeneous (!) SNIa: Light curves

1994D 1996X 1992A Spectra are homogeneous

Summary of SNIa Observational properties: fairly homogeneous M B ≈M V =-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 Thermonuclear disruption of CO WDs which accreted their mass up to the Chandrasekhar limit via mass transfer from a companion in binary systems. Interpretation: Thermonuclear disruption of CO WDs which accreted their mass up to the Chandrasekhar limit via mass transfer from a companion in binary systems.

SN II: Light curves Patat et al. 1994

SNII: Spectral variety IIP IIL IIn IIpec IIb 1987A 1980K 1988Z 1997cy 1993J

56 Ni  56 Co  56 Fe SN Ib/c: Light curves Elmhamdi et al. 2004

type II type Ib SN 1993J Barbon et al. 1995

Summary 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 Interpretation : The core collapse in massive stars (M≥8M) at the end of a series central nuclear burnings which end up with the formation of an iron core. Interpretation : The core collapse in massive stars (M≥8M  ) at the end of a series central nuclear burnings which end up with the formation of an iron core. variable envelope size and mass variable 56 Ni mass variable CSM density and distribution

SN classification II

Fields of study of SNe and their host galaxies SNe in isolated galaxies, in pairs and in groups of galaxies (Petrosian & Turatto 1995, Navasardyan et al. 2001) SNe in isolated galaxies, in pairs and in groups of galaxies (Petrosian & Turatto 1995, Navasardyan et al. 2001) SNe in active and star forming galaxies (Turatto et al. 1989, Petrosian & Turatto 1990, 1992, Petrosian et al. 2005, Hakobyan 2008) SNe in active and star forming galaxies (Turatto et al. 1989, Petrosian & Turatto 1990, 1992, Petrosian et al. 2005, Hakobyan 2008) Radial distribution of CC SNe in spiral galaxies (Hakobyan et al. 2008a) Radial distribution of CC SNe in spiral galaxies (Hakobyan et al. 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 galaxies. Navasardyan et al. (2001) : To investigate the influence of environment on SN production. The aim: To investigate the influence of environment on SN production. 22 SNe in 18 isolated galaxies 22 SNe in 18 isolated galaxies 48 SNe in 40 galaxies members of 37 pairs 48 SNe in 40 galaxies members of 37 pairs 211 SNe in 170 galaxies members of 116 groups. 211 SNe in 170 galaxies members of 116 groups.

SNe in isolated galaxies, in pairs and in groups of galaxies Conclusions: Radial distributions of CC SNe in galaxies located in different environments are similar. Radial distributions of CC SNe in galaxies located in different environments are similar. SNe discovered in pairs show isotropic azimuthal distributions and do not favor a particular direction with respect to the companion galaxy. SNe discovered in pairs show isotropic azimuthal distributions and do not favor a particular direction with respect to the companion galaxy. SN rate in galaxies members of pairs is ̴ 40% higher than in average galaxy and ̴ 60% higher than in members of groups. SN rate in galaxies members of pairs is ̴ 40% higher than in average galaxy and ̴ 60% higher than in members of groups. With the possible exception of strongly interacting systems the host environment has no influence of SN production. With the possible exception of strongly interacting systems the host environment has no influence of SN production.

SNe in active and star forming (A/SF) galaxies. List 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 hosts of SNe. To compare integral properties (morphology, luminosity etc.) of the 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 search Markarian galaxies (Petrosian et al. 2007) 1544 Markarian galaxies (Petrosian et al. 2007) 1544 Second Byurakan Survey galaxies 1401 Second Byurakan Survey galaxies 1401 NGP +30 o zone A/SF galaxies (Petrosian et al. 2008) 303 NGP +30 o zone A/SF galaxies (Petrosian et al. 2008) 303 NGP +30 o zone Normal galaxies (Petrosian et al. 2008) 878 NGP +30 o zone Normal galaxies (Petrosian et al. 2008) 878 Discovered SNe Discovered SNe In Markarian galaxies 47 SNe in 41 galaxies In 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 galaxies A/SF NGP galaxies 26 SNe in 23 galaxies Normal NGP galaxies 32 SNe in 29 galaxies Normal NGP galaxies 32 SNe in 29 galaxies

The rate of SNe in A/SF and Normal galaxies. Previous results The rate of SNe in Markarian galaxies does not differ from the corresponding value of normal galaxies (Turatto et al. 1989). The rate of SNe in Markarian galaxies does not differ from the corresponding value of normal galaxies (Turatto et al. 1989). The rate of SNe in the hosts of AGNs does not differ from the corresponding value of normal galaxies (Petrosian & Turatto 1992). The rate of SNe in the hosts of AGNs does not differ from the corresponding value of normal galaxies (Petrosian & Turatto 1992). The rates of SNe Ia, II and Ib/c in SB galaxies are similar to those measured in normal galaxies (Richmond et al. 1998). The rates of SNe Ia, II and Ib/c in SB galaxies are similar to those measured in normal galaxies (Richmond et al. 1998). SNe rates in the hosts of AGNs are not enhanced (Cappellaro et al. 1999). SNe rates in the hosts of AGNs are not enhanced (Cappellaro et al. 1999). The rate of SNe Ia is increasing toward galaxies with higher activity of star formation (Mannucci et al. 2003). The rate of SNe Ia is increasing toward galaxies with higher activity of star formation (Mannucci et al. 2003).

The rate of SNe in A/SF and Normal galaxies Petrosian et al. (2005) Frequency per luminosity unit (SNu) a with standard errors: __________________________________________________________________ Mrk A/SF Normal Cappellaro et al. (1999) Mrk A/SF Normal Cappellaro et al. (1999)__________________________________________________________________ Ntot 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) 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 (10 10 Lo(B)) -1

The rate of SNe in A/SF and Normal galaxies. Conclusions The rates of SN Ia and CC SN in A/SF galaxies are higher than in the galaxies of the control sample. The rates of SN Ia and CC SN in A/SF galaxies are higher than in the galaxies of the control sample. 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.

Morphologies of SNe hosts Mean values: SNIa – 2.5±2.1(28) SNII+Ib/c – 4.2±2.5(32) K-S Probability of Morphology Distribution (distributions are the same) : - 12% same) : - 12%

Morphologies of SNe hosts. Conclusions SNe Ia have been discovered in all galaxy types. SNe Ia have been discovered in all galaxy types. CC SNe are discovered only in spiral and irregular galaxies. CC SNe are discovered only in spiral and irregular galaxies.

Radial distribution of SNe Previous results The radial distributions of SNe Ia and SNe II are similar (Bartunov et al. 1992). The radial distributions of SNe Ia and SNe II are similar (Bartunov et al. 1992). SNe Ia are more centrally concentrated than SNe II (Howell & Wheeler 1999 ). SNe Ia are more centrally concentrated than SNe II (Howell & Wheeler 1999 ). The radial distribution of SNe Ia is in general different from those of CC SNe (Wang et al. 1997): The radial distribution of SNe Ia is in general different from those of 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 Bergh 1997). SNe Ib/c may be more centrally concentrated than SNe II (van den Bergh 1997).

Radial distribution of SNe Mean values: SNIa – 0.49±0.26(24) SNII – 0.59±0.31(22) SNIb/c – 0.31±0.18(10) K-S Probability of Radial Distribution (distributions are the same) : SNe Ia/II - 20%

Radial distribution of SNe. Conclusions The radial distribution of SNe Ia is in general different from those of CC SNe. The radial distribution of SNe Ia is in general different from those of CC SNe. There is a relative excess of SNe II compared to SNe Ia events near the very center of the galaxy. There is a relative excess of SNe II compared to SNe Ia 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 regions. Previous results SNe of all types are concentrated towards spiral arms (Bartunov et al. 1994). SNe of all types are concentrated towards spiral arms (Bartunov et al. 1994). CC SNe are tightly concentrated in spiral arms; SNe Ia show looser concentration (Maza & van den Bergh 1996). CC SNe are tightly concentrated in spiral arms; SNe Ia show looser concentration (Maza & van den Bergh 1996). SNe Ia are not correlated with the HII regions (Bartunov et al. 1994). SNe Ia are not correlated with the HII regions (Bartunov et al. 1994). SNe II and Ib/c show strong and not significantly different association with HII regions (e.g. Van Dyk et al. 1996). SNe II and Ib/c show strong and not significantly different association with HII regions (e.g. Van Dyk et al. 1996).

Distribution of SNe relative to spiral arms and HII regions. Conclusions 39% of SNe Ia and 72% of CC SNe are concentrated to the spiral arms. 39% of SNe Ia and 72% of CC SNe are concentrated to 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. 1996). (71% 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) SNe total sample N = 59 SNe total sample N = 59 SNe Ia sample N= 22 SNe Ia sample N= 22 CC SNe N = 32 CC SNe N = 32 Parameters in use: Parameters in use: Morph, AL, M(B), R(Kpc), Inc, R(SN)/R(25), SN type

Multivariate Factor Analysis (MFA). Conclusions SNe Ib/c more prefer to be discovered in A/SF hosts than SNe II and significantly more than SNe Ia. SNe Ib/c more prefer to be discovered in A/SF hosts than 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 the nuclei of normal galaxies!!!!! SNe Ia are closer to the nuclei of A/SF galaxies than to the 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. Hakobyan (2008) The aim: Correlation between CC SNe properties and integral parameters of their hosts. The aim: Correlation between CC SNe properties and integral parameters of their hosts. The ASC sample: 271 SNe (203 SNe II & 68 SNe Ib/c) in 243 hosts. The ASC sample: 271 SNe (203 SNe II & 68 SNe Ib/c) in 243 hosts. The method: MFA with parameters – Morph, Bar, AL, M(B), R(Kpc), Inc, SN type & R(SN)/R(25). The method: MFA with parameters – Morph, Bar, AL, M(B), R(Kpc), Inc, SN type & R(SN)/R(25).

ASC: CC SNe and their host galaxies Conclusions: –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 stronger for SNe Ib/c.

The radial distribution of CC SNe in spiral hosts Hakobyan et al. (2008a) The aim: Comparative study of relative radial distribution of CC SNe in spiral galaxies with the distribution of stars and ionized gas in spiral disks. The aim: Comparative study of relative radial distribution of CC SNe in spiral galaxies with the distribution of stars and ionized gas in spiral disks. The ASC sample: 219 CC SNe (160 SNe II and 59 SN Ib/c) in 198 spiral hosts (I < 50° The ASC sample: 219 CC SNe (160 SNe II and 59 SN Ib/c) in 198 spiral hosts (I < 50°; v< km s. v< km s -1 ).

The radial distribution of CC SNe in host spiral galaxies Conclusions: Conclusions: –The scale length of CC SNe distribution is significantly smaller than that of the stars, but consistent with that of HII regions. –SNe Ib/c have significantly smaller scale length than SNe II. –These tendencies have no significant correlations with galaxies integral parameters.

Summary of conclusions of our studies With the exception of strongly interacting systems the host environment has no influence of SN production. With the exception of strongly interacting systems the host environment has no influence of 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 stronger for SNe Ib/c. CC SNe in A/SF hosts are more centrally concentrated than in normal hosts. Latter effect is stronger for SNe Ib/c. Above tendencies have no significant correlations with the integral parameters of host galaxies. Above tendencies have no significant correlations with the integral parameters of host galaxies.

Early type galaxies with CC SNe Hakobyan et al. (2008b) Among morphologically classified hosts of CC SNe 22 have been classified as E or S0 (van den Bergh et al. 2002, 2003, 2005; ASC). Among morphologically classified hosts of CC SNe 22 have been classified as E or S0 (van den Bergh et al. 2002, 2003, 2005; ASC). Results of our study: Results of our study: –17 are misclassified spirals –1 is misclassified irregular –1 is misclassified ring galaxy –2 are mergers –NGC2768 is Elliptical galaxy 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 Progress : Multipurpose study of 3838 galaxies selected from the common southern field of Five SNe, DENIS, 2MASS, POSS-II and SERC surveys The particular aim of the study: To determine the rates of SN Ia and CC SNe calibrated to the unit mass and stellar population and relation to integral and nuclear properties of the host galaxies and their local and far environment. The particular aim of the study: To determine the rates of SN Ia and CC SNe calibrated to the unit mass and stellar population and relation to integral and nuclear properties of the host galaxies and their local and far environment. The sample: 3838 galaxies in common field of five SNe, DENIS, 2MASS, POSS-II and SERC surveys. Newly determined morphologies and measured optical and near-IR parameters. The sample: 3838 galaxies in common field of five SNe, DENIS, 2MASS, POSS-II and SERC surveys. Newly determined morphologies and measured optical and near-IR parameters.

Samples in different photometric bands Galaxies monitored SNe discovered In hosts U B R I J H K Projects in Progress: Multipurpose study of 3838 galaxies selected from the common southern field of Five SNe, DENIS, 2MASS, POSS-II and SERC surveys

Projects in Progress: SNe in corotation rings of spiral galaxies NGC4579 (SABb; Sy1.9) Corotation radius: The radius in which angular velocity of forming spiral arm density wave and the galactic disk are equal. Corotation radius: The radius in which angular velocity of forming spiral arm density wave and the galactic disk are equal. Enhanced SF in corotation ring. Enhanced SF in corotation ring. The aim: Enhanced SF and nature of different type of SNe. The aim: Enhanced SF and nature of different type of SNe. The sample: 77 SNe (53 CCSN; 9 SNIa) in 37 hosts. The sample: 77 SNe (53 CCSN; 9 SNIa) in 37 hosts.

Projects in Progress: Optical and near-IR surface photometry of SNe environments The motivations: – Surrounding stellar population can provide information about nature of SNe progenitors. – Possible detection of SNe light echoes (Sparks 1994, Boffi et al. 1999). The sample: 158 (v < km s -1 i < 50°) spiral hosts with 183 SNe (53 SN Ia, 95 SN II, The sample: 158 (v < km s -1 ; 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 (v r = 1584km s -1 ) SN1990K (IIP) in NGC150 (v r = 1584km s -1 )