Light Curves of Akn 564
- Time-binned X-ray light curves
- UV light curves
- Optical light curves
- Data:
[Spectroscopic light curve, blue region]
[Spectroscopic light curve, red region]
- Reference: Shemmer, O., et al. 2001, ApJ, 561, 162
[Abstract]
- Format of Data:
Blue table:
- Column (1): JD - 2450000
- Column (2): 4900 Å Flux in units of
10-16 ergs s-1 cm-2 Å.
- Column (3): Uncertainty in 4900 Å flux,
same units as column (2).
- Column (4): Hbeta flux in units of
10-14 ergs s-1 cm-2.
- Column (5): Uncertainty in Hbeta flux, same units as
column (4).
- Column (6): 5200 Å Flux in units of
10-16 ergs s-1 cm-2 Å.
- Column (7): Uncertainty in 5200 Å flux,
same units as column (6).
- Column (8): Origin of data (see Table 1 of Shemmer et al.).
Red table:
- Column (1): JD - 2450000
- Column (2): 6600 Å Flux in units of
10-16 ergs s-1 cm-2 Å.
- Column (3): Uncertainty in 6600 Å flux,
same units as column (2).
- Column (4): Halpha flux in units of
10-14 ergs s-1 cm-2.
- Column (5): Uncertainty in Halpha flux, same units as
column (4).
- Column (6): 6900 Å Flux in units of
10-16 ergs s-1 cm-2 Å.
- Column (7): Uncertainty in 6900 Å flux,
same units as column (6).
- Column (8): Origin of data (see Table 1 of Shemmer et al.).
- Optical photmetric light curves
- Optical light curves: scaled for cross-correlation analysis
- Data:
[Continuum at 4900 Å]
[Continuum at 5200 Å]
[Continuum at 6600 Å]
[Continuum at 6900 Å]
[H alpha]
[H beta]
- Reference: Shemmer, O., et al. 2001, ApJ, 561, 162
[Abstract]
- Format of Data:
- Column (1): JD - 2450000
- Column (2): Flux in relative units.
- Column (3): Uncertainty in flux, same units as column (2).
- Additional Notes:
For the blue sets (4900Å,
4900Å,Hbeta), there are 60 data points made up of 25 MDM and 35 Wise
spectra. The red set is based on 35 measurements from Wise spectra.
The light curves were processed as follows:
- For each continuum band a constant host flux contribution of
F = 24 × 10-16
ergs s-1 cm-2 Å-1
was subtracted (following PSF measurements done on
Wise images).
- All the Hbeta points were assigned with a relative flux uncertainty
of 3.6%.
- All the fluxes were then transformed into relative flux units
by dividing each flux by the mean flux of a given light curve.
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Updated 20 November 2001
peterson@astronomy.ohio-state.edu