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SNe-Ia with JDEM: Preliminary estimates

SNe-Ia with JDEM: Preliminary estimates. Massimo Della Valle & Pippus Mannucci INAF-Napoli and ESO & INAF-Arcetri. Assumptions. 2h of integration time, S/N =5 limiting (Vega) magnitudes: J= 25.85 H= 24.53 I= 26.52 R= 27.16 No other filters were available.

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SNe-Ia with JDEM: Preliminary estimates

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  1. SNe-Ia with JDEM: Preliminary estimates Massimo Della Valle & Pippus Mannucci INAF-Napoli and ESO & INAF-Arcetri

  2. Assumptions 2h of integration time, S/N =5 limiting (Vega) magnitudes: J= 25.85 H= 24.53 I= 26.52 R= 27.16 No other filters were available. 1.2m  1.5m, 2h  ~ 1h (3000s)

  3. Spectral Distribution Energy(Panagia 2003)

  4. M_B = -19.46 +-0.56, Richardson et al. 2002).

  5. Hold in check what we are doing…… Perlmutter et al. 1998 SN 1992A moved at z=0.8 after normalization to -19.46 in the B band: R=24.27 I= 23.26 SN1997ap z=0.83 R = 24.10 ± 0.09 I = 23.20 ± 0.07

  6. Assumptions 2h of integration time, S/N =5 limiting (Vega) magnitudes: J= 25.85 H= 24.53 I= 26.52 R= 27.16 No other filters were available. 1.2m  1.5m, 2h  ~ 1h (3000s)

  7. Cappellaro et al. 1997

  8. SN rates SN rates (Ia and II) from Cappellaro et al. 1999, Mannucci et al. 2005 SNe / yr deg^2 dz z

  9. 700 SNe-Ia / yr deg2 SNe / yr deg 2

  10. MDVP 2007

  11. 700 SNe-Ia / yr deg2 dust 550 SNe-Ia / yr deg2 SNe / yr deg 2

  12. Botticella et al. 2008 400-800 SNe-Ia / yr deg2

  13. 700 SNe-Ia / yr deg2 dust 550 SNe-Ia / yr deg2 1000 SNe-Ia/yr deg2 up to z ~2 SNe / yr deg 2

  14. ESO HAWK+VLT J=23.9 H=22.5 K=22.3 3600s and S/N=5

  15. z=1

  16. Summary • The SN survey  in J band  range of redshifts of cosmological interest (up to z ~ 1.5). Survey in I (or R) bands are less deep (z~1-1.2). • The estimated number of detectable SNe-Ia, up to z~1.5 (after correction for dust) is ~ 550 SNe-Ia /yr deg2 (400-800). After assuming a survey efficiency of ~ 0.5, the number of detected SNe-Ia over 4 deg2 and 2yr of mission turns out to be ~ 2200 SNe. • Spectroscopic observations from JDEM telescope. • The size of the mirror represents the major drawback. Low resolution observations R=100 (still sufficient to make SN classification) are viable for z ~1 (1h). • In principle SNe-Ia are detected up to z ~ 2 (1000/yr/deg2). • Are they useful? (EELT, JWST follow up? Photometric classification) • To do list: i) to carry out similar computations for II, Ib/c and HNe ii) to explore the possibility to observe SNe-Ia at near-IR wavelengths (rest frame)

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