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SNe-Ia with JDEM:Preliminary estimates

Massimo Della Valle & Pippus Mannucci

INAF-Napoli and ESO & INAF-Arcetri

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AssumptionsAssumptions

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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)

Spectral Distribution EnergySpectral Distribution Energy(Panagia 2003)(Panagia 2003)

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

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SN 1992A moved at z=0.8 after normalization to -19.46 in the B band:

R=24.27I= 23.26

Perlmutter et al. 1998

SN1997ap

z=0.83

R = 24.10 ± 0.09I = 23.20 ± 0.07

Hold in check what we are doing……

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AssumptionsAssumptions

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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)

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11Cappellaro et al. 1997

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SN

e /

yr d

eg^2

dz

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

SN rates

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SN

e /

yr d

eg 2

700 SNe-Ia / yr deg2

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MDVP 2007

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SN

e /

yr d

eg 2

700 SNe-Ia / yr deg2 dust 550 SNe-Ia / yr deg2

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Botticella et al. 2008

400-800 SNe-Ia / yr deg2

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SN

e /

yr d

eg 2

700 SNe-Ia / yr deg2 dust 550 SNe-Ia / yr deg2 1000 SNe-Ia/yr deg2 up to z ~2

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ESO HAWK+VLTJ=23.9H=22.5K=22.3

3600s and S/N=5

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z=1

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• 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)

Summary