ACS Coronagraphic Imaging ETC

This form will calculate the count rates and S/N ratio for a simulated spectrum of ONE source in an ACS coronographic imaging observation. For general help on how to use this Exposure Time Calculator or for help on various topics, click on the appropriate highlighted words. You may also like to see the current known release notes.

1. Select one Camera and the associated Filter(s):

Instrument Mode:

Detector Filter Wheel 1 Filter Wheel 2
HRC

Select an occulting spot

Target acquisition mode (no occulting spot, no central source)

1.8 arc second diameter

3.0 arc second diameter

2. Specify the exposure parameters:

Exposure time needed to obtain a S/N ratio of
S/N ratio reached in an exposure time of seconds.

Select the source type and photometric extraction aperture (centered on the target) that will be used for the S/N ratio calculation:


Point Source
Use the default region for the camera selected, a circular region containing 80 percent of total light.
Use a square region of size:
Use a circular region of radius (arcsec):
Use a circular region of radius (arcsec):
Use a circular region containing percent of total light. The range of supported values for this option is limited. The limits are determined by the PSF and target spectrum.

Extended Source
Diameter is arcsec
Use the default extraction aperture (square of 2x2 pixels)
Use a square extraction region of size (pixels):
Use a circular region of radius (arcsec):

3. Choose one of the following spectral distributions for the reference (field) source:

Please note: for User supplied and uploaded spectrum, please use only FITS or text format files.


Upload Spectrum File:
Other HST Spectrum:
CDBS Synphot spectrum file
Castelli and Kurucz Models: [Sp Teff log(g) log(z)=0]
Pickles Models: (Sp Teff)
Kurucz Models:
Bruzual Synthetic Stellar Spectra:
HST Standard Star spectra:
Non-Stellar Objects:
a Black-body with temperature T =
a Power-law: Fλ = λ **
a Flat continuum in
No continuum. If selected, at least one emission line must be specified below, and the reference wavelength from part 2 above must correspond to one of the lines.

Specify the extinction E(B-V) =

Extinction applied normalization.

Specify the redshift z =

Add emission lines to the input spectrum (optional):

Line Center FWHM Integrated Flux
(Å) Å (erg/cm2/s)
(vacuum)

Note: integrated flux units are per arcsec2 for extended sources. All three of the parameters (line center, fwhm and integrated flux) must be specified for an emission line to be included.

4. Normalize the target's flux:

= (Vega magnitudes) (arcsec-2 for extended sources) or
ergs cm-2 s-1 Å-1 (arcsec-2 for extended sources) at Å. or
Do not Renormalize Point Source Spectrum. Use only for User Input Spectrum or Calibration Spectra.

5. Specify the expected background levels :

a) Specify normalization for zodiacal background
Standard zodiacal light normalizations:
Compute zodiacal light on sky position:
R.A.: (hh:mm:ss or decimal)
Dec.: (dd:mm:ss or decimal)
either λ - λSun: degrees
- or - Date:
Normalize zodiacal light to magnitude:
Scale zodiacal light by factor (1.56 = average):
b) Specify normalization for earth shine background
Standard earth shine light normalizations:
Normalize earth shine light to magnitude:
Scale earth shine light by factor (0.5 = average):
c) Air Glow

Separation: arcsec

5a. Choose one of the following spectral distributions for the central (occulted) source:

Please note: for User supplied and uploaded spectrum, please use only FITS or text format files.


Upload Spectrum File:
Other HST Spectrum:
CDBS Synphot spectrum file
Castelli and Kurucz Models: [Sp Teff log(g) log(z)=0]
Pickles Models: (Sp Teff)
Kurucz Models:
Bruzual Synthetic Stellar Spectra:
HST Standard Star spectra:
Non-Stellar Objects:
a Black-body with temperature T =
a Power-law: Fλ = λ **
a Flat continuum in
No continuum. If selected, at least one emission line must be specified below, and the reference wavelength from part 2 above must correspond to one of the lines.

Specify the extinction E(B-V) =

Extinction applied normalization.

Specify the redshift z =

= (Vega magnitudes) (arcsec-2 for extended sources) or
ergs cm-2 s-1 Å-1 (arcsec-2 for extended sources) at Å. or
Do not Renormalize Point Source Spectrum. Use only for User Input Spectrum or Calibration Spectra.

6. Additional CCD parameters:

Gain Setting CR-SPLIT