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IFU Studies of GRBs and SNe Regions

Explore the connection between GRBs and SNe regions, focusing on the fireball model, core collapse explosion types, progenitor stars, and host galaxy studies. Comparison of IFU data with archive data reveals insights on properties and metallicities in GRB/SNe regions. Ongoing studies aim to uncover systematic differences in metallicity and upgrade VIMOS detectors for future investigations.

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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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