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IFU studies of GRBs and SNe regions

IFU studies of GRBs and SNe regions. Lise Christensen (Excellence Cluster Universe, Technical University Munich) + Maryam Modjaz (NY), + Christina Thoene (IAA, Granada),

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IFU studies of GRBs and SNe regions

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  1. IFU studies of GRBs and SNe regions Lise Christensen (Excellence Cluster Universe, Technical University Munich) + Maryam Modjaz (NY), + Christina Thoene (IAA, Granada), + Susanna Vergani (INAF, Brera) + Aybuke Yoldas (IOA, Cambridge)

  2. What makes a GRB? Fireball model

  3. GRBs/SNe connection SN bump Type Ic Hjorth et al. 2003 Bloom et al. 1999

  4. Core collapse explosion types Type II : + H Type Ib : - H + He Type Ic : - H - He - Si binary mass transfer? Type Ic broad lined(hypernova): - H – He Ekin >1052 erg (model dependent) line widths: ~30 000 km/s no GRB GRB / Ic –bl : metal poor : <10% solar, fast rotating GRB/ no SN Ic –bl ( SN detections are the exception – Fynbo+ 2006) Yoon et al. 2006

  5. Host galaxy studies • What makes a GRB/ hypernova? – • We never spotted a progenitor • of a Type Ib/c SN • Clues from their hosts: • Progenitor star mass • Stellar population age • Metallicity • proximity to HII regions

  6. HST images of hosts of long duration bursts at z=1 (Fruchter et al 2006)

  7. Redshift/host magnitude distribution Jakobsson et al. 2010

  8. Host of GRB 980425 - SN 1998 bw (z=0.0085) HST WFPC FORS BVR VIMOS cube 30” = 5 kpc • Compare IFU- with archive data: • Magnitudes and colours have to match broad band data • Extracted narrow band IFU image has to match Ha narrow band images • IFU extracted spectra have to match long slit spectra

  9. GRB 980425 host: Derived properties • Ha emission line fit - > velocity map -> dynamicmass • Ha flux -> SFR, Specific SFR <- 24 m Spitzer image • Ha flux / continuum -> Ha EW -> age • Ha/Hb -> reddening E(B-V) • Flux ratios [OIII]/Hb / [NII]/Ha  Oxygen abundance • Each spectrum > stellar population fitting -> stellar mass,age • GRB region is not so • unusual 12+log(O/H) Christensen et al 2008

  10. GRB 060505 (z=0.08) VIMOS cube FORS - R • GRB site: • No SN detected • young: 6 Myrs = 32 M star • metal poorer than the galaxy • (slit spectra) • progenitor likely a • massive star Thoene et al. 2010

  11. Unusual emission line ratios? 980425 051117B E(B-V)=0.5, solar metallicity Models: Dopita et al. 2006

  12. Metallicities In GRB/SNe regions Modjaz et al. 2008

  13. GRB – SN connections SN/GRB location in host Metallicity distribution Modjaz et al. 2010 But disagrees with Anderson et al. 2010 Kelly et al 2008

  14. NGC 6754: 4 SNe in 10 years Type Ia Type II Type Ia N NICMOS,F110W, FOV~50” Type II

  15. New VIMOS detectors Old: 30-40% level detector fringes New: ~10% IFU fringes in some spectra (also present In old data)

  16. New VIMOS detector sensitivities Q1 Q2 Q3 Q4 new old

  17. Future studies of SNe hosts • Type Ic / Ic –bl (without GRBs) • Targeted / non-targeted galaxies • Sample of ~ 20 galaxies • (Current status: applied for observations) MB= -21 to -18

  18. Ongoing studies of GRB hosts VLT 2010 - IFU programmes: Low-z hosts with Sinfoni + AO : High spatial resolution on four closest hosts Stellar population in the GRB site ~100 pc (Z, age, mass) (PI: A. Yoldas) High-z : Sinfoni – No AO: locate galaxies in line of sight (Mg II absorbers) faint emission from GRB hosts (PI: S. Vergani) GRB 021004 (z=2.33) [O III] 5007

  19. Summary • Aim: to distinguish GRB and SN regions from host studies • Systematic differences in metallicity between GRB and SNe • Unusual regions in hosts – maybe for GRBs, but unknown for SNe Ic’s • Only looked systematically at HII region emission lines (GRB/SNe) • Underlying stellar populations to be investigated (GRB/SNe) • Upgrade of VIMOS detectors is promising for future studies

  20. GRB 060505 - questioningthe GRB-SN connection • z=0.08 • shortishduration: 4s • no SN detected in lightcurve at verydeep limits • (norwithspectroscopy) • Located in large star-formingregion

  21. Higher spectral resolution Flames- ARGUS archive data R~10000 Courtesy: M. Dessauges-Zavadsky + F. Hammer

  22. Global metallicity in SN hosts Modjaz et al. 2010

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