If this issue still exists for you can you set logging to debug level (The 'Logs' button In EKOS next to where you start or connect to INDI, tick Verbose and File and Filter Wheel.) then try moving the filter wheel from EKOS again and post the debug logs so that we can have a look.
Hi Michel, Yes, setting the temperature and pressure for the mount to use to correct for refraction is in there. (the :SRTMP and :SRPRS commands)
These can be seen in the screenshot I posted in the first two rows.
Obviously something still needs to provide real temperature and pressure measurements, but the driver can at least set them in the mount.
Hi Michel, I'm not exactly sure what you mean, the driver so far is just an interface to the 10Micron API meaning that :newalpt wants the plate solved J2000 coordinates to be corrected for precession, nutation and light aberration in JNow, but not corrected for refraction in any way.
I would like to add the J2000->JNow(precession, nutation and light aberration) to INDI by adding (parts of) ERFA to INDI, but that would also make INDI quite a bit larger and I doubt 'the other INDI devs' want that.
I've added basic alignment building to the driver. I want to test it first before making a pull request to merge it into the main INDI tree. I hope that my skies allow for that soon
plan makes sense. will be a lot of work too
maybe extend (1) with upgrading KStars/EKOS ?
and at (3) explain clearly which keys or menu options to use
And this whole thing will need an index of some sort
For 10Micron mount modelling we need to add the following functionality to the driver :
First store the temperature and pressure. This will get used by :newalpt and/or :endalig# lateron.
- :SRTMPsTTT.T# Sets the tempreature at the location of the telescope used in the refraction model to sTTT.T degrees Celsius. Returns 1# if OK, 0# on error.
- :SRPRSPPPP.P# Sets the atmospheric pressure at the location of the telescope used in the refraction model to PPPP.P hPa. Returns 1# if OK, 0# on error.
- :newalig# returns V#
- :GR# get mount right ascension. Returns HH:MM:SS.SS# (hours, minutes, seconds and hundredths of seconds)
- :GD# get mount declination. Returns sDD:MM:SS.S# (degrees, arcminutes, arcseconds and tenths of arcsecond)
- :pS# Pier side. Returns string "East#" or "West#"
- :GS# Get local sidereal time
- :newalptMRA,MDEC,MSIDE,PRA,PDEC,SIDTIME# Returns nnn# if OK with nnn the number of active points, E# if not
- MRA - the mount-reported right ascension, expressed as HH:MM:SS.S
- MDEC - the mount-reported declination, expressed as sDD:MM:SS
- MSIDE - the mount-reported pier side (the letter 'E' or 'W', as reported by the :pS# command)
- PRA - the plate-solved right ascension (i.e. the right ascension the telescope was effectively pointing to), expressed as HH:MM:SS.S
- PDEC - the plate-solved declination (i.e. the declination the telescope was effectively pointing to), expressed as sDD:MM:SS
- SIDTIME - the local sidereal time at the time of the measurement of the point, expressed as HH:MM:SS.S
- :endalig# returns V# if new alignment model has been computed OK
- :modeldel0NAME# DELete a model with name NAME (up to 15 case sensitive characters, spaces allowed). Returns 1# if OK, 0# on error
- :modelsv0NAME# SaVe the model with name NAME. Returns 1# if OK, 0# on error
The 10Micron mount then receives these 'half transformed' coordinates and corrects for refraction with the temperature and pressure it was given earlier with :SRTMP and :SRPRS (ignoring things like humidity and wavelength).
Lateron we can add functionality to manage the models with these
- :getalst# Gets the number of alignment stars used in the current alignment model. Returns n#
- :delalig# Deletes the current alignment model and stars. Returns #
- :getalpN# Gets alignment information for star number N. Returns: E# on error or "HH:MM:SS.SS,+dd*mm:ss.s,eeee.e,ppp#" where HH:MM:SS.SS is the hour angle of the alignment star in hours, minutes, seconds and hundredths of second (from 0h to 23h59m59.99s), +dd*mm:ss.s is the declination of the alignment star in degrees, arcminutes, arcseconds and tenths of arcsecond, eeee.e is the error between the star and the alignment model in arcseconds, ppp is the polar angle of the measured star with respect to the modeled star in the equatorial system in degrees from 0 to 359 (0 towards the north pole, 90 towards east).
- :delalstN# Delete alignment star N and recalculate the model. Returns 1# if OK, 0# on error
- :modelcnt# Gets the number of alignment models. Returns: n#
- :modelnamN# Returns the name of model number N or just # on error.
- :modelld0NAME# Loads the model with the given NAME. Returns 1# if OK, 0# on error
I intend to add all this to the INDI driver. Does this line up with the EKOS Mount Modelling tool ?
mworion wrote: ... With the SOFA library I would do a C to python translation myself over time if there is no solution available. First I have to ask the guys at SOFA to get the allowance to use it in MountWizzard.
I propose to use ERFA instead : github.com/liberfa/erfa "ERFA is a C library containing key algorithms for astronomy, and is based on the SOFA library published by the International Astronomical Union (IAU).
ERFA is intended to replicate the functionality of SOFA (aside from possible bugfixes in ERFA that have not yet been included in SOFA), but is licensed under a three-clause BSD license to enable its compatibility with a wide range of open source licenses. Permission for this release has been obtained from the SOFA board, and is avilable in the LICENSE file included in this source distribution."
I've tested ERFA myself and it gives the same results as SOFA github.com/d33psky/J2000-JNow
Hi all, I'm glad to see 10Micron mount modeling is getting more attention in INDI/EKOS-land.
The 10-Micron mount alignment models are made in the mounts themselves and are based on (currently up to 100) alignment points. The interesting case is where we plate solve these points so that the whole procedure can be automated. The INDI Alignment Subsystem could be used to select those points, have them plate solved and add the results as a new alignment point to the mount. This is what Michel's MountWizzard does too (it does a lot more).
The mount also wants temperature and air pressure information as it uses this to correct for their effects on pointing. A 'fun fact' is that we must not correct for temperature and air pressure ourselves when converting the plate solved J2000 results to JNow (confirmed to me by a 10Micron dev).
We should use the 10-Micron :newalig# , :newalpt , :endalig# commands to build models instead of just :CM# to 'sync' a point. Next step is to let the mount evaluate the model, optimize it and maybe remove certain points that show too large errors. I do not know if IAS has something similar. The mount can save and recall multiple alignment models.
Ideally I would like to see both MountWizzard and EKOS be able to help build 10Micron alignment models from Linux/Mac/Windows. MountWizzard is mostly Python and it would be really nice if it could be fully Python based. There are INDI client implementations in pure Python so that could be used. The J2000-JNow transformation it currently uses via ASCOM is based on SOFA with a mix of NOVAS helper functions ... I know of no Python-only library of it yet.