MATISSE in the VLTI context
The VLTI delivers four input beams to MATISSE, from either the four ATs or the four UTs. Each beam has been stabilized with an adaptive optics system in the telescope (NAOMI or MACAO, respectively), and an the residual tip-tilt due to effects downstream from the telescope is measured in the VLTI lab by IRIS and applied through the AO system as well. Since the target acquisition is performed with IRIS, the respective limits apply. For details see the VLTI manual.
The instrument is currently largely stand-alone from the infrastructure of the VLTI. As such it does not use external fringe-tracking, and only acts as a coherencer, meaning it will only center the entire fringe package after a number of exposures, but does not keep the individual fringes in position. A coherent adding up of indivdual exposures is therefore only possible if the fringes can be centered in each exposure, or if assumptions on the fringe movements are made. The use of GRAVITY as an external fringe tracker for MATISSE is being investigated.
The CIAO adaptive optics system for the UTs is currently not offered for MATISSE.
MATISSE Optical Elements
The following is a general description of the optical path, for more detail and numerical information see the instrument manuals.
On the warm optics bench, the beams pass through two commuting devices that can interchange the input beams 1 vs. 2 and 3 vs. 4, respectively. They are always used, and any observation consists of at least one BCD-IN and one BCD-OUT measurement. Comparing the BCD-IN with the BCD-OUT data enables correction of instrumental chromatic effects on the measured interferometric phases.
After the LM- and N-bands have been separated on the wam optics part, the beams enter the LM or N-band cryostat. The internal setup of each cryostat is comparable, so this general description is applicable to both cryostats. In an intermediate focus the beams pass through a spatial filter, either a slit or a pinhole, with defined size of the order of the point-spread function. ESO has chosen a standard setup for those, but expert users in visitor mode can make use of the alternative options.
When the photo-interferometric splitter is inserted into the beam, source photometry and fringes are observed simultaneously (SIPHOT mode), otherwise they have to be taken sequentially (HISENS mode). Currently the only offered option is to observe L-band in SIPHOT and N-band in HISENS, which is the so-called HYBRID mode.
Users experienced with N-band interferometry might wish to use the correlated flux measurement provided by MATISSE instead of the full visibility information. Since a correlated flux measurement does not require that source photometry is obtained, the execution time per OB is shorter, and correlated fluxes can be obtained for fainter sources than full visibility measurements. However, in that case the user must have information about at least the calibrator flux from an external source, and preferably the science target as well. Correlated flux measurements are not possible in the LM-band.
The dispersive optics provides a choice of several resolving powers. Filters to reduce the total background are inserted according to the chosen spectral resolution and wavelength range. The polarizing filters are not available for scientific observations.
Calibrators and Calibration Strategy
MATISSE if offered with two observing sequences, either CAL-SCI or CAL-SCI-CAL.
Calibrator stars for N-band and L-band can be found, for instance, with the SearchCal tool provided by the jmmc (see links). However, finding a star that is suitable for both bands at the same time can be tricky. Users should make sure already at phase 1, i.e. for proposal submission, that their chosen calibration strategy is possible and suitable calibrators are available. In case no good L+N calibrators are nearby, the user should consider to use the CAL-SCI-CAL sequence with one calibrator for L-band and one for N-band. The following recommendations should be considered when choosing a calibrator star:
- Prefer to use the JMMC-SearchCal Tool instead of ESO-CalVin, since the latter is currently not updated.
- Mid-IR fluxes are hard to measure. It is recommended to compute median fluxes in L and N bands using for example the VizieR Photometry viewer provided by CDS-SIMBAD intead of relying on a single source.
- Good calibrators should follow the Rayleigh-Jeans approximation, i.e., avoid IR excess. L/N-band flux ratio (at 3.3 and 8.5 microns) should best be within a range of 7 to 9.
- A SIMBAD search on the calibrator should show "star" as object type.
- A calibrator catalogue is in preparation by the MATISSE consortium. For further information please contact the consortium.
MATISSE in P103
MATISSE is offered in period 103 based on early commissioning results. Hence only a subset of functions and modes will be available to the user, and the inital limiting magnitudes and conditions will likely be revised for some of the setups for later periods.
- Hybrid is the only observing mode offered.
- L-band observations are offered with low (R=34), medium (R=506), and high (R=959), but not very high resolution in P103.
- M-band observations are not offered in P103.
- N-band observations are offered with low resolution (R=30) only in P103.
- The DIT values are fixed. The chosen DIT for L-band enables to observe a spectral window of about 0.1 micrometer in high resolution, and 0.2 micrometer in medium resolution, which the user can center freely.
|L-band low||20 min||40 min||60 min|
|L-band medium||20 min||40min||60 min|
|L-band high||25 min||50 min||75 min|
|N-band photometry||+10 minutes||+20 minutes||+30 minutes|
Sensitivity and Errors vs. Observing Conditions
The target flux brackets below are defined in such a way that the typical errors for
- low resolution observations will be better than 5 degrees on closure phase data and better than10% on absolute visbilities
- medium resolution obervation will be better than 10 degrees for closure phase data and better than 20% on absolute visbilities
- attempting to obtain absolute calibrated quantities with high resolution is not recommended.
- medium and high resolution observations will be about 1 degree on differential phases, and better than 10% on differential visibilities.
However, bad observing conditions do not only diminish the flux. If a science case is critically dependent to achieve the best possible error bars, it is strongly recommended to request good observing conditions regardless of the target brightness. Observations at seeing values worse than 1.2" are not recommended.
|Seeing < 0.8", CLR||Seeing < 1.2", THN||Seeing < 0.8", CLR||Seeing < 1.2", THN|
|L-band low||3 Jy||5 Jy||0.5 Jy||1 Jy|
|L-band medium||20 Jy||30 Jy||2 Jy||3 Jy|
|L-band high||75 Jy||115 Jy||8 Jy||12 Jy|
|N-band low, full visibilities||20 Jy||30 Jy||2 Jy||4 Jy|
|N-band low, correlated fluxes only||5 Jy||10 Jy||1 Jy||2 Jy|