Observation index table¶
The observation index table is stored in a FITS file as a BINTABLE HDU:
- Suggested filename:
obs-index.fits.gz
- Suggested HDU name:
OBS_INDEX
It contains one row per observation (a.k.a. run) and lists parameters that are commonly used for observation selection, grouping and analysis.
Required columns¶
OBS_ID
type: int- Unique observation identifier (Run number)
RA_PNT
type: float, unit: deg- Obsevation pointing right ascension (see RA / DEC)
DEC_PNT
type: float, unit: deg- Observation pointing declination (see RA / DEC)
ZEN_PNT
type: float, unit: deg- Observation pointing zenith angle at observation mid-time
TMID
(see Alt / Az)
- Observation pointing zenith angle at observation mid-time
ALT_PNT
float, deg- Observation pointing altitude at observation mid-time
TMID
(see Alt / Az)
- Observation pointing altitude at observation mid-time
AZ_PNT
type: float, unit: deg- Observation pointing azimuth at observation mid-time
TMID
(see Alt / Az)
- Observation pointing azimuth at observation mid-time
ONTIME
type: float, unit: s- Total observation time (including dead time).
- Equals
TSTOP
-TSTART
LIVETIME
type: float, unit: s- Total livetime (observation minus dead time)
DEADC
type: float- Dead time correction.
- It is defined such that
LIVETIME
=DEADC
*ONTIME
i.e. the fraction of time the telescope was actually able to take data.
TSTART
type: float, unit: days- Start of observation in MJD
TSTART_STR
type: string- Start of observation in UTC string format: “YYYY-MM-DD HH:MM:SS”
TSTOP
type: float, unit: days- End time of observation in MJD
TSTOP_STR
type: string- End of observation in UTC string format: “YYYY-MM-DD HH:MM:SS”
N_TELS
type: int- Number of participating telescopes
TELLIST
type: string- Telescope IDs (e.g. ‘1,2,3,4’)
QUALITY
type: int- Observation data quality. The following levels of data quality are defined:
- 0 = best quality, suitable for spectral analysis.
- 1 = medium quality, suitable for detection, but not spectra (typically if the atmosphere was hazy).
- 2 = bad quality, usually not to be used for analysis.
Optional columns¶
The following columns are optional. They are sometimes used for observation selection or data quality checks or analysis, but aren’t needed for most users.
OBJECT
type: string- Primary target of the observation
- Recommendations:
- Use a name that can be resolved by SESAME
- For survey observations, use “survey”.
- For Off Observation, use “off observation”
RA_OBJ
type: float, unit: deg- Right ascension of
OBJECT
- Right ascension of
DEC_OBJ
type: float, unit: deg- Declination of
OBJECT
- Declination of
TMID
type: float, unit: days- Mid time of observation in MJD (=
TSTART
+ 0.5 *ONTIME
)
- Mid time of observation in MJD (=
TMID_STR
type: string- Mid time of observation in UTC string format: “YYYY-MM-DD HH:MM:SS”
EVENT_COUNT
type: int- Number of events in run
EVENT_RA_MEDIAN
type: float, unit: deg- Median right ascension of events
EVENT_DEC_MEDIAN
type: float, unit: deg- Median declination of events
EVENT_ENERGY_MEDIAN
type: float, unit: deg- Median energy of events
EVENT_TIME_MIN
type: double, unit: s- First event time
EVENT_TIME_MAX
type: double, unit: s- Last event time
BKG_SCALE
type: float- Observation-dependent background scaling factor. See notes below.
TRGRATE
type: float, unit: Hz- Mean system trigger rate
ZTRGRATE
type: float, unit: Hz- Zenith equivalent mean system trigger rate
- Some HESS chains export this at the moment and this quantity can be useful for data selection. Comparing values from different chains or other telescopes would require a more specific specification.
MUONEFF
type: float- Mean muon efficiency
- Currently use definitions from analysis chain, since creating a unified specification is tricky.
BROKPIX
type: float- Fraction of broken pixels (0.15 means 15% broken pixels)
AIRTEMP
type: float, unit: deg C- Mean air temperature at ground during the observation.
PRESSURE
type: float, unit: hPa- Mean air pressure at ground during the observation.
NSBLEVEL
type: float, unit: a.u.- Measure for NSB level
- Some HESS chains export this at the moment and this quantity can be useful for data selection. Comparing values from different chains or other telescopes would require a more specific specification.
RELHUM
type: float- Relative humidity
- Definition
Notes¶
- This table doesn’t require header keywords. We recommend FITS is used, but it can be stored e.g. in CSV as well.
- Some of the required columns are redundant. E.g.
ONTIME
=TSTOP
-TSTART
. The motivation to declare those columns required is to make it easy for users and tools to browse the observation lists and select observations via cuts on these parameters without having to compute them on the fly. - Observation runs where the telescopes don’t point to a fixed RA / DEC position (e.g. drift scan runs) aren’t supported at the moment by this format.
- Times are given as a UTC string or MJD float.
This is preferred over the use of mission elapsed time (MET),
because MET requires a reference timepoint stored in header keywords
MJDREFI
andMJDREFF
, and we felt that having a simpler table format here that doesn’t require a header would be nice. - Purpose / definition of
BKG_SCALE
: For a 3D likelihood analysis a good estimate of the background is important. The run-by-run varation of the background rate is ~20%. The main reasons are the changing atmospheric conditions. This parameter allows to specify (from separate studies) a scaling factor to the Background This factor comes e.g. from the analysis of off runs. The background normalisation usually dependends on e.g. the number of events in a run, the zenith angle and other parameters. This parameter provides the possibility to give the user a better prediction of the background normalisation. For CTA this might be induced from atmospheric monitoring and additional diagnostic input. For HESS we try to find a trend in the off run background normalisations and other parameters such as number of events per unit livetime. The background scale should be around 1.0 if the background model is good. This number should also be set to 1.0 if no dependency analysis has been performed. If the background model normalisation is off by a few orders of magnitude for some reasons, this can also be incorporated here.