European Southern Observatory
New Technology Telescope

General :
Observations :

SUSI2

Photometric Throughput Evolution

Evolution

The following figure displays the evolution of the count rates (in electron/s, atmosphere corrected) for a mag=15 star, for the 5 standard filters, as well as the corresponding zero point. Significant events have been indicated as labels. This page is generated automatically. The photometric reduction is performed using the Tmag Midas package.

Detector Set-Up:	Fast, bin 2x2
Counts:	10^4 e-/sec, airmass=0, M=15
Zero Points:	adu, airmass=0

PostScript

Last automatic update: Wed Jul 31 19:47:50 SAT 2002

NTT Team: updtate procedure in www: ~/Photometry/susiZP/README

Photometric Solution

Typical photometric solutions

U = u + 23.52 -airm*0.35 +0.10*(U-B)

B = b + 25.46 -airm*0.22 -0.22*(B-V)

V = v + 25.74 -airm*0.13 -0.02*(V-R)

R = r + 25.61 -airm*0.09 -0.05*(R-I)

I = i + 24.61 -airm*0.07 -0.10*(R-I)

M: standard magnitude, m: instrumental magnitude (adu/s)

The archive of photometric solutions is available as an ascii file. However, before using these values blindly, remember that the Zero Points depend on the flat-field you used, or, more specifically, of the region used for the normalisation.

Send comments to: NTT Webmasters <nttweb@www.ls.eso.org>
Last Update: 2001-Dec-31 (oh.)