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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

SNe-Ia with JDEM:

Preliminary estimates

Massimo Della Valle & Pippus Mannucci

INAF-Napoli and ESO & INAF-Arcetri


Assumptions
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)




Sne ia with jdem preliminary estimates

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


Assumptions1
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)



Sne ia with jdem preliminary estimates

SN rates

SN rates (Ia and II) from Cappellaro et al. 1999, Mannucci et al. 2005

SNe / yr deg^2 dz

z


Sne ia with jdem preliminary estimates

700 SNe-Ia / yr deg2

SNe / yr deg 2



Sne ia with jdem preliminary estimates

700 SNe-Ia / yr deg2 dust

550 SNe-Ia / yr deg2

SNe / yr deg 2


Sne ia with jdem preliminary estimates

Botticella et al. 2008

400-800 SNe-Ia / yr deg2


Sne ia with jdem preliminary estimates

700 SNe-Ia / yr deg2 dust

550 SNe-Ia / yr deg2

1000 SNe-Ia/yr deg2 up to z ~2

SNe / yr deg 2


Sne ia with jdem preliminary estimates

ESO HAWK+VLT

J=23.9

H=22.5

K=22.3

3600s and S/N=5



Sne ia with jdem preliminary estimates

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)