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Deep Surveys for Supernovae …. and other variable objects

Deep Surveys for Supernovae …. and other variable objects. Massimo Turatto. INAF. Overview:. why intermediate/high-z SN surveys ? where to focus planned SN surveys LBC (only) surveys? precursor programs. No mention to SN/GRB and other exotic SNe. High-z team.

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Deep Surveys for Supernovae …. and other variable objects

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  1. Deep Surveys for Supernovae…. and other variable objects Massimo Turatto INAF LBT Bertinoro 2002

  2. Overview: • why intermediate/high-z SN surveys ? • where to focus • planned SN surveys • LBC (only) surveys? • precursor programs • No mention to SN/GRB and other exotic SNe LBT Bertinoro 2002

  3. High-z team 1-Determination of the cosmological parameters SNIa + CMB anisotropyw. Boomerang & MAXIMA LBT Bertinoro 2002

  4. Open questions 1 Cosmological parameters • Diversity • Contamination • Extinction • Evolution • Statistics/Accuracy LBT Bertinoro 2002

  5. Calibration of SN Ia absolute magnitude Absolute light curves of 87 SN Ia LBT Bertinoro 2002

  6. Hamuy et al. (1996) Mmax vs. light curve shape Hamuy et al. 1996 LBT Bertinoro 2002

  7. Hubble diagram Hamuy et al. 1996 LBT Bertinoro 2002

  8. Altavilla et al. 2002 • slope ? • dispersion ? LBT Bertinoro 2002

  9. m15 vs. galaxy type Inaccurate m15 correction  systematic error @ high-z Cappellaro et al. 2001 LBT Bertinoro 2002

  10. early color curve of SNIa outer layers  progenitor structure/composition LBT Bertinoro 2002

  11. Contamination = GRB280498 MV LBT Bertinoro 2002

  12. Contamination Ia template SN 1992ar Ic z = 0.15 LBT Bertinoro 2002

  13. Contamination SN 1992ar Ic z = 0.15 Ia Ia LBT Bertinoro 2002

  14. Contamination SN 1992ar Ic z = 0.15 Ic Ic LBT Bertinoro 2002

  15. Interstellar Extinction (younger Universe) NaID galactic hostgalaxy LBT Bertinoro 2002

  16. empirical E(B-V) vs.EW(NaID) -EW(NaID) measured -E(B-V) from Ia late colors (Phillips et al. 1999) - galactic (Schlegel et al. 1998) LBT Bertinoro 2002

  17. accuracy Δm 0.25 mag LBC VST /statistics LBT Bertinoro 2002

  18. 2-Determination of the SF history II (tot) II (S) Ia (tot) Ia (S) II (E) Ia (E) Hamuy et al.1999 Pain et al.1999 Cappellaro et al.1997 Pain et al.1996 Altavila et al. 2002 Pain et al.2000 Hardin et al. 2000 Reiss 2000 Kobayashi, Nomoto, Tsujimoto astro-ph/0102247 LBT Bertinoro 2002

  19. Open questions 2 - Rate • Uneven sampling • CCSNe missing • Designed strategy • Contamination by exotics (SN/GRB, …) LBT Bertinoro 2002

  20. CFHT Legacy Survey 450 nights over 5 years, with MegaCam, a 40-CCD 1degx1deg camera • A very wide shallow survey. Ecliptic (+/-2  degrees), outer SS population beyond Neptune + our Galaxy, 3 bands and 2 epochs. • A wide synoptic survey. 172 sq. degrees, 4 bands to i'=24.5, large scale structures and matter distribution. 2 epochs. • A deep synoptic survey. 4 sq. degrees, 4 filters . 1n every 4 for 5 years Goal: • dark energy • transient phenomena and moving objects.  starting now detection and monitoring of 2000 SNIa LBT Bertinoro 2002

  21. ESSENCE • Mosaic Imager on the Blanco 4-m • 50 fields • 30x1/2n per yr over 5 yr (complementary/synergy to Supermacho) • 0.15 < z < 0.75. • VRI + zJ and spectra (Keck, MMT, Magellan, Gemini, VLT) • “self-contained” • AIM: Equation of State of the Universe starting now 200 SNIa LBT Bertinoro 2002

  22. Supernova / Acceleration Probe Goal: • Mmax vs. z for 2000 SNIa up to z=1.7 • restframe B band (9 equivalent bands) • classification and z from spectroscopy Instrument concept (evolving): Mirror: 2m equivalent Field: 0.6 sq. degree Range: 350-1700nm Detectors: LBNL CCD 0.10”/px, HgCdTe 0.17”/px Duration: 3 yr Cadence: 4d LBT Bertinoro 2002

  23. SNAP baseline Starting ???? IFU Image slicer LBT Bertinoro 2002

  24. Large-aperture Synoptic Survey telescope 8.4m primary mirror 6.9m effective aperture 7 square degree field 55cm diameter focal surface 24th mag in 20 sec > 5 Tbyte/night Real-time analysis LBT Bertinoro 2002

  25. 200 000 SNe 3000 high-z SNe • all-sky survey: • every ~7days • 1 band • m~24 • deep survey: • 100 sq degrees • m~26 • n bands In operation starting 2010 ?? LBT Bertinoro 2002

  26. LBC: Blue and Red arms Optics + MAT 42-90 detectors of LBC LBT Bertinoro 2002

  27. band drift Example: z=0.9, mIa,max = 24.5(Ho=65, M=0.3, =0.7) direct comparison IB small Kcrossband correction B I QE=0.70 I restframe z=0.9 LBT Bertinoro 2002

  28. LBC can do it easily !! discover … + characterize !! m15 Extremely rare (HST) High-z team LBT Bertinoro 2002

  29. Poznanski et al. astro-ph/0202198 …. grey polygon includes almost all stars, cataclysmic variables, Cepheids, asteroids and quasars …… LBT Bertinoro 2002

  30. Stritzinger et al. 2002 Turatto 2002 UV flash in Core Collapse SNe LBT Bertinoro 2002

  31. 22.4 26.4 30.4 22.4 26.4 30.4 Chugai et al. 2000 Blue/Reddeep SN search (alone) with proper sampling discovers & classifies Type Ia (cosmology) and CC-SNe (rate) up to z1 CC-SN UV flash @ high-z B LBT Bertinoro 2002

  32. Expected number of SNe Dahlén&Fransson 1999A&A,350 349 Number of SNe per field 150 50 1.5 0.15 sq.degr. field LBT Bertinoro 2002

  33. Southern Intermediate Redshift ESO SN Search(STRESS) WFI@2.2m Telescope aperture: 2.2 m Field of view: 34`x 33` Pixel scale: 0.238 arcsec/pix • surveyed area ~5.1 sq degr • spectroscopic follow up 12 nights ESO 2.2+WFI 6 nights FORS1/2 LBT Bertinoro 2002

  34. LBT Bertinoro 2002

  35. Subtraction steps: • geometric and photometric alignment • best PSF image convolution • subtraction • (ISIS Alard & Lupton 1998 ApJ 503, 325 ) Image to be searched Reference image Subtracted image SN 2000fc type Ia V=22.4 z=0.42 IAUC7537 Each image is the sum of three 15min exposures Examples of spectra LBT Bertinoro 2002

  36. SNe spectroscopically confirmed(200 candidates) Altavilla et al. 2002 LBT Bertinoro 2002

  37. Preliminary results and comparison with data in literature Rate (SNu, scaling as (H0/75)2) z N.SNe Ia Ib IIreferences local 83 0.25 0.28 Cappellaro et al. 1993 A&A 268, 472 local 31 0.28 Hamuy & Pinto 1999 AJ 117, 1185 local 137 0.20 0.08 0.40 Cappellaro et al. 1999 A&A 351, 459 ~0.10 4 0.25 Hardin et al. 2000 A&A 362, 419 ~0.20 5 0.20 0.27 Altavilla et al. 2002 ~0.40 3 0.46 Pain et al. 1996 ApJ 473, 356 ~0.55 38 0.51 Pain et al. Astro-ph/0205476 a: 3 Ia + 2 II, considering the SNe of our subsample (13 SNe) with redshift 0.15<z<0.25 b: values uncorrected for absorption c: model E b b +0.40 -0.17 +0.06 -0.06 +0.04 -0.04 +0.19 -0.19 +0.27 -0.16 +0.20 b -0.18 +0.28 b -0.25 a +0.51 -0.35 +0.15 c -0.13 LBT Bertinoro 2002

  38. … more variable objects LBT Bertinoro 2002

  39. public LBT Bertinoro 2002

  40. once a new candidate is detected LBT Bertinoro 2002

  41. history of all variable sources  AGN LBT Bertinoro 2002

  42. variable stars NEO AGN SNe LBT Bertinoro 2002

  43. lesson learnt about LBT • LBC will play a key role in SN science of the next few yr • (FoV, BRarms, timing) • WF SN search is demanding • feasible even in competitive environment (ESO) • remunerative despite big effort • strategy is crucial • interesting additional science …. all other instruments as well LBT Bertinoro 2002

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