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Local Universe Supernovae and Their Host Galaxies

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

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Local Universe Supernovae and Their Host Galaxies

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  1. 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

  2. Historical Milky Way Supernovae • The earliest recorded SN185 in 185AD. • The Crab Nebula associated with the  1054 supernova • Tyco’s Nova SN1572 • Kepler's supernova Remnant, SN 1604  • G1.9+0.3: Youngest (~140 yr) known SN

  3. Extragalactic Supernovae SN 1998S • First extragalactic SNe (S Andromedae) was discovered in Andromeda galaxy in 1885. • In 1934 Baade & Zwicky (1934) define supernovae as separate class of objects. • First systematic SN search was initiated by Zwicky in 1936. • Currently the number of discovered SNe is approaching to 5000 from which about 50% have been discovered in 21st century.

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

  5. Taxonomy 2003 Turatto 2003

  6. Classification of SupernovaeTuratto 2003

  7. SNIa: Light curves Light curves are homogeneous (!)

  8. Spectra are homogeneous 1994D 1996X 1992A

  9. Summary 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 accreted their mass up to the Chandrasekhar limit via mass transfer from a companion in binary systems.

  10. SN II: Light curves Patat et al. 1994

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

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

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

  14. 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 56Ni mass • variable CSM density and distribution 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

  15. SN classification II

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

  17. SNe in isolated galaxies, in pairs and in groups of galaxies. Navasardyan et al. (2001) • The aim: To investigate the influence of environment on SN production. • 22 SNe in 18 isolated galaxies • 48 SNe in 40 galaxies members of 37 pairs • 211 SNe in 170 galaxies members of 116 groups.

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

  19. 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 determine the rates of SNe in A/SF and normal galaxies. • To compare integral properties (morphology, luminosity etc.) of the hosts of SNe. • To determine the radial distribution of SNe in spiral galaxies. • To determine SNe and spiral arms connection. • To study association of SNe with SF regions.

  20. The samples of galaxies for SNe search • Markarian galaxies (Petrosian et al. 2007) 1544 • Second Byurakan Survey galaxies 1401 • NGP +30o zone A/SF galaxies (Petrosian et al. 2008) 303 • NGP +30o zone Normal galaxies (Petrosian et al. 2008) 878 Discovered SNe • In Markarian galaxies 47 SNe in 41 galaxies • SBS galaxies 10 SNe in 6 galaxies (5 Mrks) • A/SF NGP galaxies 26 SNe in 23 galaxies • Normal NGP galaxies 32 SNe in 29 galaxies

  21. 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 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). • 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).

  22. The rate of SNe in A/SF and Normal galaxiesPetrosian et al. (2005) Frequency per luminosity unit (SNu)a with standard errors: __________________________________________________________________ Mrk A/SF Normal Cappellaro et al. (1999) __________________________________________________________________ Ntot 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) 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) __________________________________________________________________ a1SNu = 1SN(100Yr) -1 (1010Lo(B)) -1

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

  24. 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%

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

  26. Radial distribution of SNePrevious results • 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 ). • 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 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 may be more centrally concentrated than SNe II (van den Bergh 1997).

  27. 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%

  28. Radial distribution of SNe. Conclusions • 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. • SNe Ib/c are more centrally concentrated than SNe Ia. • SNe Ib/c are more centrally concentrated than SNe II.

  29. 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). • 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 II and Ib/c show strong and not significantly different association with HII regions (e.g. Van Dyk et al. 1996).

  30. 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. • There is no SNe Ia associated with HII region. • 68% of CC SNe are associated with the HII regions (71% Van Dyk et al. 1996). • 20% of CC SNe are close to the nuclear regions (< 0.17).

  31. Multivariate Factor Analysis (MFA) • SNe total sample N = 59 • SNe Ia sample N= 22 • CC SNe N = 32 • Parameters in use: Morph, AL, M(B), R(Kpc), Inc, R(SN)/R(25), SN type

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

  33. ASC: CC SNe and their host galaxies.Hakobyan (2008) • 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 method: MFA with parameters – Morph, Bar, AL, M(B), R(Kpc), Inc, SN type & R(SN)/R(25).

  34. 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.

  35. The radial distribution of CC SNe in spiral hostsHakobyan 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 ASC sample: 219 CC SNe (160 SNe II and 59 SN Ib/c) in 198 spiral hosts (I < 50°; v< 10000 km s-1).

  36. The radial distribution of CC SNe in host spiral galaxies • 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.

  37. Summary of conclusions of our studies • 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. • 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. • 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. • 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.

  38. Early type galaxies with CC SNeHakobyan 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). • 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.

  39. 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).

  40. 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 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.

  41. Projects in Progress: Multipurpose study of 3838 galaxies selected from the common southern field of Five SNe, DENIS, 2MASS, POSS-II and SERC surveys Samples in different photometric bands

  42. Projects in Progress: SNe in corotation rings of spiral galaxiesNGC4579 (SABb; Sy1.9) • 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. • The aim: Enhanced SF and nature of different type of SNe. • The sample: 77 SNe (53 CCSN; 9 SNIa) in 37 hosts.

  43. 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 < 10000 km s-1;i < 50°) spiral hosts with 183 SNe (53 SN Ia, 95 SN II, 35 SN Ib/c). SN1990K (IIP) in NGC150 (vr = 1584km s-1)

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