1. Standard Imaging pipeline specification¶
1.1. Association Diagram¶
1.2. MICADO Dataitems¶
Summary of all Raw Instrument Data observed in imaging mode. |
||||||
|DPR keywords |
||||||
Name |
Description |
CATG |
TECH |
TYPE |
DO.CATG |
|
I_DARK_RAW |
Detector exposure without illumination (via block in pupil filter wheel and field restrictor). |
CALIB |
IMAGE,SI |
DARK |
RAW_DARK |
|
I_FLAT_RAW |
Raw exposure using the flatfield lamp in imaging mode. |
CALIB |
IMAGE,SI |
FLAT,LAMP |
RAW_OPT_FLAT |
|
I_NONLIN_RAW |
Raw exposure using the flatfield lamp in imaging mode for non-linearity correction. |
CALIB |
IMAGE,SI |
NONLIN,LAMP |
RAW_OPT_NONLIN |
|
I_ILLUM_RAW |
Raw Science data for Illumination correction. |
CALIB |
IMAGE,SI |
STD,ILLUM |
RAW_OPT_SKY_ILLUM |
|
I_STDFIELD_RAW |
Raw data for Photometric Zerpoint determination. |
CALIB |
IMAGE,SI |
STD,PHOTOM |
RAW_OPT_SKY_STDFIELD |
|
I_BKGFIELD_RAW |
Raw data for background determination. |
CALIB |
IMAGE,AI |
OBJECT,BCKGRND |
RAW_OPT_SKY_BKGFIELD |
|
I_SCI_RAW |
Raw on-sky exposure. |
SCIENCE |
IMAGE,SI |
OBJECT,SKY |
RAW_OPT_SKY_SKYSIAI_SCIENCE |
|
I_SCI_CORO_WAFFLE_RAW |
Focal plane image of bright star with waffle pattern added. |
SCIENCE |
CORONOGRAPHY,WAFFLE |
OBJECT |
RAW_OPT_SKY_SKYHCI_CORO_SCIENCECOROWAFFLE |
|
I_CORO_OFFSET_RAW |
Image on bright point source with coronagraph in place. Star must be offset from coronagraph. |
CALIB |
CORONOGRAPHY |
STAR |
RAW_OPT_SKY_SKYHCI_CORO_COROOFFSET |
|
I_SCI_CORO_PUPIL_RAW |
Pupil plane mask HCI image. |
SCIENCE |
CORONOGRAPHY |
PUPIL |
RAW_OPT_SKY_SKYHCI_CORO_SCIENCECOROPUPIL |
|
I_CORO_BGD_RAW |
Background sky image for the science images (and online processing). |
CALIB |
CORONOGRAPHY |
BACKGROUND |
RAW_OPT_SKY_SKYHCI_CORO_COROBACKGROUND |
|
I_SCI_AI_RAW |
Raw on-sky exposure for astrometric imaging. |
SCIENCE |
IMAGE,AI |
OBJECT,SKY |
RAW_OPT_SKY_SKYSIAI_SCIENCEAI |
|
I_WAM_RAW |
Raw warm astrometric mask data for distortion determination. |
CALIB |
IMAGE,AI |
PINHOLE,WAM |
RAW_OPT_WAMCAM_WAM |
|
I_CAM_RAW |
Raw cold astrometric mask data for distortion determination. Not used in the automatic pipeline. |
CALIB |
IMAGE,AI |
PINHOLE,CAM |
RAW_OPT_WAMCAM_CAM |
|
I_ASTROMFIELD_RAW |
Raw data for distortion determination. |
CALIB |
IMAGE,SI |
STD,ASTROMETRY |
RAW_OPT_SKY_ASTROMFIELD |
Summary of all External DataItems for imaging. |
|||
|PRO keywords |
|||
Name |
Description |
DO.CATG |
|
REF_I_ASTROM_CAT |
Catalog with (ra,dec) of on-sky astrometric reference standards. Input surveys: Gaia and Euclid. |
CAT_DISTORTIONREF_ASTROMREF |
|
REF_I_PHOTOM_CAT |
Catalog with magnitudes of a photometric reference standards in a series of filters. Input surveys: JWST, Euclid YJH, VISTA surveys. Such catalogs are input for determination of zeropoints and/or illumination correction. |
CAT_PHOTOMREF |
|
REF_I_WAM_CAT |
Catalog with reference positions of the warm astrometric mask pinholes. |
CAT_DISTORTIONREF_WAMREF |
Summary of all Intermediate and Final Data for imaging. |
|||
|PRO keywords |
|||
Name |
Description |
DO.CATG |
|
I_ASTROM_HDR |
Astrometric solution. One per detector. |
HDR_ASTROM |
|
I_BGD_IMG |
Background per detector. |
IMG_BACKGROUND |
|
I_MASTER_DARK_IMG |
MasterDark calibration image. |
IMG_MASTERDARK |
|
I_MASTER_FLAT_IMG |
Flatfield image obtained by combining a series of internal flatfield lamp observations. |
IMG_MASTERFLAT |
|
I_DT_SCI_SI_IMG |
Image which has been corrected for instrumental effects, not background subtracted. |
IMG_FNL_CATALOGABLE_DT_DTSIAI_DT |
|
I_DTFNL_SCI_IMG |
Image which has been corrected for instrumental effects, and background subtracted. |
IMG_FNL_CATALOGABLE_DTFNL_DTFNLSIAI_DTFNL |
|
I_ILLUM_CORR_HDR |
Table with the coefficients of the polynomial describing the large-scale variation in the illumination by the flatfield lamp, and gain (e-/ADU), which is a single number per detector. |
HDR_STATICTABLE_ILLUMCORR |
|
I_PERSISTENCE_IMG |
Persistence image. |
IMG_PERSISTENCE |
|
I_PHOTOM_HDR |
Zeropoint and extinction coefficient, one pair per detector. |
HDR_PHOTOM |
|
I_SCI_STACK_IMG |
Coaddition of calibrated images. |
IMG_STACK |
|
I_DT_SCI_CORO_WAFFLE_IMG |
Waffle image which has been corrected for instrumental effects for HCI, and background subtracted. |
IMG_FNL_CATALOGABLE_DT_DTHCI_DTWAFFLE |
|
I_DT_SCI_CORO_PUPIL_IMG |
Pupil image which has been corrected for instrumental effects for HCI, and background subtracted. |
IMG_FNL_CATALOGABLE_DT_DTHCI_DTPUPIL |
|
I_STARCENTER_WAFFLE_HDR |
Table with the star center during the OB on the detector. The position is in pixel units in the Pixel Grid Coordinate System. Derived from waffle pattern. |
HDR_STARCENTER_STARCENTERWAFFLE |
|
I_STARCENTER_PUPIL_HDR |
Table with the star center during the OB on the detector. The position is in pixel units in the Pixel Grid Coordinate System. |
HDR_STARCENTER_STARCENTERPUPIL |
1.3. MICADO Pipeline¶
1.4. MICADO Recipes¶
1.4.1. I_PERSISTENCE_IMG¶
Purpose:
null
Algorithm and workflow:
null
Name |
Persistence |
ReqID |
None |
Parent ReqID |
None |
Objective |
Determine the persistence correction for an exposure. |
Responsible |
ESO |
Phase |
N/A |
MICADO Set-up |
N/A |
Calibration Unit setup |
N/A |
Observing Template |
N/A |
Template parameters |
N/A |
Frequency |
N/A |
Duration estimate [s] |
N/A |
Prerequisites |
N/A |
Recipe frequency |
Once for each exposure. (Possibly batched.) |
Input data |
|
Output products |
|
QC parameters |
None |
DRL Recipe ID |
micado_det_persistence |
Procedure |
Use the HDRL routine developed by Mark Neeser. |
Mathematical description |
See proposal by Mark Neeser. |
Remarks |
Currently under development by ESO. This recipe will be primarily be ran by ESO since it requires all previous data (up till a certain time in the past), including proprietary data. It can also be ran by users after the proprietary period is over. |
Accuracy |
Measurement uncertainty 10%. Systematic error 10%. |
1.4.2. I_MASTER_DARK_IMG¶
Purpose:
Darks will be used for the dark current correction and requires the same exposure time as the science data. Thus, these frames have to be taken on daily basis, but during day time.
Algorithm and workflow:
The observation template MCD_img_cal_dark provides N dark frames, which are median or mean combined to create the MASTERDARK_IMG frame. The input frames have to be taken with the same exposure time as the SCIENCE exposures.
Name |
Master Dark |
ReqID |
DPS-masterdark |
Parent ReqID |
R-MCD-100 |
Objective |
Determine the dark current and flag hot pixels. |
Responsible |
Science Operations |
Phase |
Daytime |
MICADO Set-up |
|
Calibration Unit setup |
Not active |
Observing Template |
MICADO_img_cal_dark |
Template parameters |
INS.MODE, INS.READMODE, DET.DIT, DET.NDIT, INSTRUME |
Frequency |
daily |
Duration estimate [s] |
4654 |
Prerequisites |
None |
Recipe frequency |
Once per Observing Block with dark frames. |
Input data |
|
Output products |
|
QC parameters |
QC DARKMEAN, QC DARKMED, QC DARKSTD, QC NPIXSAT, QC FPIXSAT |
DRL Recipe ID |
micado_det_dark |
Procedure |
Median filtering of the input exposures; hdrl_imagelist_collapse with median filtering will be used. Pixels above PAR{THRESH_UPLIM_DARK} in all input darks are flagged as hot pixels. |
Mathematical description |
hdrl_imagelist_collapse with median filtering will be used. |
Remarks |
It is expected that dark current is independent of read option. Baseline is to limit all science exposures to a finite set of exposure times. This ensures the darks, with the same finite set of exposure times, can be taken before a night instead of following it: mitigates persistence in the raw darks. |
Accuracy |
Dark current measurement uncertainty 10%. Systematic error 10% as inferred from simulated data. 90% hot pixels flagged. |
1.4.3. I_MASTER_FLAT_IMG¶
Purpose:
Algorithm and workflow:
Name |
Master Flat |
ReqID |
DPS-flatfield |
Parent ReqID |
R-MCD-100 |
Objective |
Determine pixelsensitivity variation at scale of few pixels and flag cold pixels. |
Responsible |
Science Operations |
Phase |
Daytime |
MICADO Set-up |
|
Calibration Unit setup |
Flat field lamp ON |
Observing Template |
MICADO_img_cal_flat |
Template parameters |
INS.MODE, INS.FILT1.NAME, INS.FILT2.NAME, INS.OPTI6.NAME, INS.DROT, INS.READMODE, DET.DIT, DET.NDIT, INSTRUME |
Frequency |
daily |
Duration estimate [s] |
254 |
Prerequisites |
Normal instrumental conditions. |
Recipe frequency |
Once per Observing Block with flat frames. |
Input data |
|
Output products |
|
QC parameters |
QC FLATMEAN, QC FLATMED, QC FLATSTD, QC NPIXHOT, QC FPIXHOT |
DRL Recipe ID |
micado_img_flat |
Procedure |
Subtraction of additive components followed by median/mean filtering of the input exposures. Pixels below PAR{THRESH_LOWLIM_FLAT} in all input flats are flagged as cold pixels. |
Mathematical description |
hdrl_imagelist_collapse with median filtering will be used. |
Remarks |
None |
Accuracy |
0.5% precision on pixel sensitivity, validated on simulated data. 90% cold pixels flagged. |
1.4.4. I_DT_SCI_SI_IMG¶
Purpose:
null
Algorithm and workflow:
null
Name |
First Detrend exposure step |
ReqID |
DPS-3120-SCI |
Parent ReqID |
[R-MCD-130]D/ /I/ ; [I-INS/ELT-203] / / / ; [R-INS-928] / /I/T |
Objective |
Apply to a raw exposure pixels the additive and multiplicative factors to correct for detector instrumental fingerprint. |
Responsible |
User |
Phase |
N/A |
MICADO Set-up |
N/A |
Calibration Unit setup |
N/A |
Observing Template |
N/A |
Template parameters |
N/A |
Frequency |
N/A |
Duration estimate [s] |
N/A |
Prerequisites |
N/A |
Recipe frequency |
Once for each OB with raw science (and potentially offset sky) exposures. |
Input data |
I_SCI_RAW_, I_NONLINEARITY_IMG_, I_MASTER_DARK_IMG, I_PERSISTENCE_IMG, I_MASTER_FLAT_IMG |
Output products |
|
QC parameters |
QC DETSMEAN, QC DETSMED, QC DETSSTD, QC DETRENCR, QC NPIXNONL, QC FPIXNONL |
DRL Recipe ID |
micado_img_detrend |
Procedure |
See individual steps. |
Mathematical description |
See individual steps. |
Remarks |
None |
Accuracy |
TODO |
1.4.5. I_BGD_IMG¶
Purpose:
null
Algorithm and workflow:
null
Name |
Background |
ReqID |
None |
Parent ReqID |
None |
Objective |
Determine the background of all exposures in an observation. Created either from a background field observation offset from the science observation, or directly from the science observation itself. |
Responsible |
User |
Phase |
Nighttime |
MICADO Set-up |
|
Calibration Unit setup |
Not active. |
Observing Template |
MICADO_img_obs[bg] |
Template parameters |
INS.MODE, INS.READMODE, DET.DIT, DET.NDIT, INSTRUME |
Frequency |
For each science observation that cannot be used for background determination. |
Duration estimate [s] |
varying |
Prerequisites |
Photometric conditions. Input products imply the recipes that must run prior to this recipe. |
Recipe frequency |
Once for each OB with raw science or bkgfield exposures. |
Input data |
|
Output products |
|
QC parameters |
QC BACKGROUNDMEANn, QC BACKGROUNDMEDn, QC BACKGROUNDSTDn |
DRL Recipe ID |
micado_img_background |
Procedure |
Derive background for each frame from all exposures. hdrl_collapse_imagelist_to_image_sigclip will be used. |
Mathematical description |
TODO |
Remarks |
None |
Accuracy |
TODO |
1.4.6. I_ILLUM_CORR_HDR¶
Purpose:
null
Algorithm and workflow:
null
Name |
Flatlamp illumination correction |
ReqID |
DPS-illumcorr |
Parent ReqID |
R-MCD-100 |
Objective |
Determine spatial variation in illumination by flatlamp over detector array |
Responsible |
Science Operations |
Phase |
Nighttime |
MICADO Set-up |
|
Calibration Unit setup |
Not active. |
Observing Template |
MICADO_img_tec_illum |
Template parameters |
INS.MODE, INS.READMODE, DET.DIT, DET.NDIT, INSTRUME |
Frequency |
During commissioning and after each instrument intervention. |
Duration estimate [s] |
2050 |
Prerequisites |
Photometric observing conditions. |
Recipe frequency |
Once after each instrument intervention. |
Input data |
|
Output products |
|
QC parameters |
QC ILLUNMAT, QC ILLSNRMD |
DRL Recipe ID |
micado_img_illum |
Procedure |
Use a “MICADO Photometric Reference Field” for which a catalog of at least relative stellar fluxes with sufficiently dense stellar distribution already exists. Such a catalog could be established through external data (e.g., JWST, Euclid and/or Gaia) or a one-time dedicated programme with MICADO (e.g., during commissioning). With that catalog in hand, single exposures of that field suffice to monitor variation in the illumination variation. The determination of the IllumMap is then a fit to stellar flux measurements. Whether a parametric fit suffices (e.g., polynomial of degree N) depends on the complexity of illumination variation. |
Mathematical description |
The algorithm from by href{https://doi.org/10.1007/s10686-011-9266-x}{McFarland, Verdoes-Kleijn, Sikkema, et al. Exp Astron 35, 45-78 (2013)}. |
Remarks |
These observations are on the Large Magellanic Cloud Reference Field (described in Section~ref{sec:photometricreferencestars}). The reference magnitudes have accuracies of 1% or better. This calibration task assumes a polynomial behavior of the illumination variation. |
Accuracy |
Measurement precision of 1% and accuracy of 10% on value of illumination variation value over full FoV. So if true illumination variation is 20% we want an accuracy of 20% +/-2%. |
1.4.7. I_DTFNL_SCI_IMG¶
Purpose:
null
Algorithm and workflow:
null
Name |
Final Detrend exposure step |
ReqID |
None |
Parent ReqID |
None |
Objective |
Subtract background and apply illumination correction. |
Responsible |
User |
Phase |
N/A |
MICADO Set-up |
N/A |
Calibration Unit setup |
N/A |
Observing Template |
N/A |
Template parameters |
N/A |
Frequency |
N/A |
Duration estimate [s] |
N/A |
Prerequisites |
N/A |
Recipe frequency |
Once for each OB with raw science exposures. |
Input data |
|
Output products |
|
QC parameters |
None |
DRL Recipe ID |
micado_img_detrend_final |
Procedure |
See individual steps. |
Mathematical description |
See individual steps. |
Remarks |
None |
Accuracy |
TODO |
1.4.8. I_ASTROM_HDR¶
Purpose:
This recipe requires as input several data items representing the instrumental geometric distortions. The recipes that create these data items are described in the Astrometric Imaging section.
Algorithm and workflow:
null
Name |
Astrometric solution |
ReqID |
DPS-3140-SCI |
Parent ReqID |
[R-MCD-116] /A/ /T ; [I-INS/ELT-101] / / / |
Objective |
Determine a polynomial function that maps pixel coordinates (x,y) into (RA,Dec). |
Responsible |
User |
Phase |
|
MICADO Set-up |
None |
Calibration Unit setup |
None |
Observing Template |
MCD_img_obs_siai_base |
Template parameters |
INS.MODE, OBS.RA, OBS.DEC, INS.FILT1.NAME, INS.FILT2.NAME, INS.OPTI6.NAME, INS.DROT, INS.READMODE, DET.DIT, DET.NDIT, INSTRUME |
Frequency |
None |
Duration estimate [s] |
None |
Prerequisites |
None |
Recipe frequency |
Once for each detrended science exposure. |
Input data |
I_DTFNL_SIAI_IMG_, I_DISTORTION_WAM_HDR_, I_DISTORTION_ELT_HDR_, REF_I_ASTROM_CAT_ |
Output products |
|
QC parameters |
QC DCRVALn, QC DCRVALn, QC RMSDRA, QC RMSDDEC |
DRL Recipe ID |
micado_img_astrom |
Procedure |
Plan to use procedure similar to SCAMP (Bertin 2006: ASP Conference Series, Vol. 351, 2006), HAWK-I, and VIKING. |
Mathematical description |
TODO: choose from SCAMP, HAWK-I and VIKING, e.g. SCAMP (Bertin 2006: ASP Conference Series, Vol. 351, 2006, https://www.astromatic.net/software/scamp). Add to recipe steps: differential atmospheric refraction computation available in HDRL. |
Remarks |
The plan is to use Gaia and Euclid catalogs to construct the astrometric reference catalog (ASTROMREF_CAT). |
Accuracy |
TODO |
1.4.9. I_PHOTOM_STDFIELD_HDR¶
Purpose:
null
Algorithm and workflow:
null
Name |
Photometric solution |
ReqID |
DPS-photomstandardfield |
Parent ReqID |
R-MCD-100 |
Objective |
Determine the scalar zeropoint that converts fluxes (in units of ADUs) into magnitudes at the top of the atmosphere. |
Responsible |
User |
Phase |
Nighttime |
MICADO Set-up |
|
Calibration Unit setup |
Not active. |
Observing Template |
MICADO_img_cal_zeropoint |
Template parameters |
INS.MODE, OBS.RA, OBS.DEC, INS.FILT1.NAME, INS.FILT2.NAME, INS.OPTI6.NAME, INS.DROT, INS.READMODE, DET.DIT, DET.NDIT, INSTRUME |
Frequency |
The User decides whether this Observing Block is added to its phase 2 set to derive the zeropoint independent from the science observations. By default the zeropoint is determined using reference stars inside the science images. |
Duration estimate [s] |
247 (for 1 filter) |
Prerequisites |
Photometric conditions. |
Recipe frequency |
Once per exposure of a photometric reference field. |
Input data |
|
Output products |
|
QC parameters |
QC ZPTSTDi, QC NMATCHi |
DRL Recipe ID |
micado_img_photom |
Procedure |
Procedure planned to be similar as used for HAWK-I (see ftp://ftp.eso.org/pub/dfs/pipelines/hawki/hawki-pipeline-manual-2.4.3.pdf) Include as recipe steps (i) object catalog production available in HDRL, (ii) Strehl ratio computation available in HDRL, (iii) airmass computation available in HDRL. |
Mathematical description |
Algorithm planned to be similar as used for HAWK-I (see ftp://ftp.eso.org/pub/dfs/pipelines/hawki/hawki-pipeline-manual-2.4.3.pdf) |
Remarks |
PHOTOMSTDFIELD_HDR contains zeropoint and extinction coefficient, one pair per detector. No user defined parameters by default. User can manually optimize source extraction parameters (e.g., aperture, SNR threshold reference sources). |
Accuracy |
1% measurement precision, 5% accuracy |
1.4.10. I_SCI_CALIBRATED_IMG¶
Purpose:
null
Algorithm and workflow:
null
Name |
Apply photom and astrom solution |
ReqID |
DPS-3160-SCI |
Parent ReqID |
R-INS-928] / /I/T |
Objective |
Apply the photometric and astrometric solution for exposures to the pixels. |
Responsible |
User |
Phase |
|
MICADO Set-up |
None |
Calibration Unit setup |
None |
Observing Template |
MCD_img_obs_siai_base |
Template parameters |
INS.MODE, OBS.RA, OBS.DEC, INS.FILT1.NAME, INS.FILT2.NAME, INS.OPTI6.NAME, INS.DROT, INS.READMODE, DET.DIT, DET.NDIT, INSTRUME |
Frequency |
None |
Duration estimate [s] |
None |
Prerequisites |
None |
Recipe frequency |
Once per Observing Block |
Input data |
|
Output products |
|
QC parameters |
QC CALIMEAi, QC CALISTDi |
DRL Recipe ID |
micado_img_calibrate |
Procedure |
Procedure planned to be similar as used for HAWK-I (see Section 6.6 of ftp://ftp.eso.org/pub/dfs/pipelines/hawki/hawki-pipeline-manual-2.4.3.pdf) |
Mathematical description |
Algorithm planned to be similar as used for HAWK-I (see Section 6.6 of ftp://ftp.eso.org/pub/dfs/pipelines/hawki/hawki-pipeline-manual-2.4.3.pdf) |
Remarks |
None |
Accuracy |
TODO |
1.4.11. I_SCI_STACK_IMG¶
Purpose:
null
Algorithm and workflow:
null
Name |
Stack |
ReqID |
None |
Parent ReqID |
None |
Objective |
Combine calibrated exposures into one stack. |
Responsible |
User |
Phase |
|
MICADO Set-up |
None |
Calibration Unit setup |
None |
Observing Template |
MCD_img_obs_siai_base |
Template parameters |
INS.MODE, OBS.RA, OBS.DEC, INS.FILT1.NAME, INS.FILT2.NAME, INS.OPTI6.NAME, INS.DROT, INS.READMODE, DET.DIT, DET.NDIT, INSTRUME |
Frequency |
None |
Duration estimate [s] |
None |
Prerequisites |
None |
Recipe frequency |
Once per Observing Block |
Input data |
|
Output products |
|
QC parameters |
QC STACKMEANn, QC STACKSTDn, QC STACKMEDn |
DRL Recipe ID |
micado_img_stack |
Procedure |
Procedure planned to be similar as used for HAWK-I (see Section 6.6 of ftp://ftp.eso.org/pub/dfs/pipelines/hawki/hawki-pipeline-manual-2.4.3.pdf) |
Mathematical description |
Algorithm planned to be similar as used for HAWK-I (see Section 6.6 of ftp://ftp.eso.org/pub/dfs/pipelines/hawki/hawki-pipeline-manual-2.4.3.pdf) |
Remarks |
TODO: User defined parameters: Projection point for stack. For stacking: weighting scheme in coaddition. |
Accuracy |
TODO |
1.4.12. I_DT_CORO_OFFSET_IMG¶
Purpose:
null
Algorithm and workflow:
null
Name |
Detrend high-contrast off-axis exposure |
ReqID |
DPS-3130-SCI |
Parent ReqID |
R-MCD-120]D/ /I/ |
Objective |
Apply to a raw exposure pixels observed in high-contrast imaging mode the additive and multiplicative factors to correct for detector instrumental fingerprint. |
Responsible |
User |
Phase |
Nighttime |
MICADO Set-up |
|
Calibration Unit setup |
Not active. |
Observing Template |
MICADO_coro_cal_starvisible |
Template parameters |
INS.MODE, OBS.RA, OBS.DEC, INS.FILT1.NAME, INS.FILT2.NAME, INS.OPTI6.NAME, INS.DROT, INS.READMODE, DET.DIT, DET.NDIT, INSTRUME |
Frequency |
The User decides the number of observing Templates instances added to its phase 2 Observing Blocks. |
Duration estimate [s] |
252 (per observing Template in this case) |
Prerequisites |
None |
Recipe frequency |
Once for each raw off-axis HCI exposure. |
Input data |
I_CORO_OFFSET_RAW_, I_NONLINEARITY_IMG_, I_MASTER_DARK_IMG, I_PERSISTENCE_IMG, I_MASTER_FLAT_IMG |
Output products |
|
QC parameters |
QC DETSMEAN, QC DETSMED, QC DETSSTD, QC DETRENCR, QC NPIXNONL, QC FPIXNONL |
DRL Recipe ID |
micado_img_detrend_hci |
Procedure |
See individual steps. Same as DetrendFinal except without illumination correction. |
Mathematical description |
See individual steps. |
Remarks |
Identical to DetrendHCI. |
Accuracy |
TODO |
1.4.13. I_STAROFFSET_HDR¶
Purpose:
null
Algorithm and workflow:
null
Name |
Coronagraphic star zeropoint and centroid |
ReqID |
DPS-corostarzptandcentroid |
Parent ReqID |
R-MCD-119 |
Objective |
Determine zeropoint and centroid of the central bright star. |
Responsible |
User |
Phase |
Nighttime |
MICADO Set-up |
|
Calibration Unit setup |
Not active. |
Observing Template |
MICADO_coro_cal_starvisible |
Template parameters |
INS.MODE, OBS.RA, OBS.DEC, INS.FILT1.NAME, INS.FILT2.NAME, INS.OPTI6.NAME, INS.DROT, INS.READMODE, DET.DIT, DET.NDIT, INSTRUME |
Frequency |
The User decides the number of observing Templates instances added to its phase 2 Observing Blocks. |
Duration estimate [s] |
252 (per observing Template in this case) |
Prerequisites |
None |
Recipe frequency |
Execute for each Observing Block |
Input data |
|
Output products |
|
QC parameters |
QC STAROFFSETSNRMINn, QC STAROFFSETSNRMAXn, QC STAROFFSETSNRMEDn, QC STAROFFSETSNRMEANn |
DRL Recipe ID |
micado_img_star_photom |
Procedure |
Measure throughput in calibration filter and using zeropoint for science filter and calibration filter to estimate throughput for science filter. Position of the star used to point the star on the mask determined using DPS-1700-INS information and calibration of the astrometric shift between observation with and without ND filter. |
Mathematical description |
To be added at FDR. |
Remarks |
See Section 5 in cite{MICADO-DRLD} for details of procedure and algorithm. |
Accuracy |
Accuracy of algorithm is a zeropoint better than 1% and a centroid better than 0.1 pixel in each dimension. |
1.4.14. I_CALIB_HCI_IMG¶
Purpose:
null
Algorithm and workflow:
null
Name |
Calibrated high-contrast science exposure |
ReqID |
None |
Parent ReqID |
None |
Objective |
Calculate proper angle. |
Responsible |
User |
Phase |
|
MICADO Set-up |
None |
Calibration Unit setup |
None |
Observing Template |
template |
Template parameters |
INS.READMODE, DET.DIT, DET.NDIT, INSTRUME |
Frequency |
None |
Duration estimate [s] |
None |
Prerequisites |
None |
Recipe frequency |
Once for each raw HCI science exposure. |
Input data |
|
Output products |
|
QC parameters |
QC CALIMEAi, QC CALISTDi |
DRL Recipe ID |
micado_img_calib_hci |
Procedure |
See individual steps. Same as DetrendFinal except without illumination correction. |
Mathematical description |
See individual steps. |
Remarks |
None |
Accuracy |
TODO |
1.5. MICADO Recipe Steps¶
1.5.1. mcd_img_vardqlayers_create¶
Create variance and data quality layers.
1.5.2. mcd_det_persistence_derive¶
Derive Persistence Correction.
1.5.3. mcd_det_persistence_apply¶
Apply Persistence Correction.
For each detector adapt the extensions as follows:
DATA: Subtract the DATA layer of the Persistence image.
ERR: Propagate the ERR layer of the Persistence image
assuming uncorrelated uncertainties. * DQ: XOR with the DQ layer of the Persistence image.
TODO: Ensure that the external Persistence map meets these requirements. TODO: Perhaps keep the persistence as a separate layer.
1.5.4. mcd_img_dark_apply¶
Apply MasterDark Correction.
1.5.5. mcd_img_flat_apply¶
Apply MasterFlat Correction.
1.5.6. mcd_det_dark_derive¶
Derive MasterDark.
1.5.7. mcd_img_flat_derive¶
Derive MasterFlat.
1.5.8. mcd_img_background_derive¶
Derive Background.
TODO: Describe background subtraction.
1.5.9. mcd_img_illum_derive¶
Derive illumination correction.
Creates the IllumCorr data product by applying the procedure described in ILLUMCORR_TAB recipe.
1.5.10. mcd_img_illum_apply¶
Apply illumination correction.
For each detector generate an illumination correction image and adapt the extensions as follows:
DATA: Multiply with the DATA layer of the illumination correction image.
ERR: Propagate the ERR layer of the illumination correction image
assuming uncorrelated uncertainties. * DQ: Nothing.
1.5.11. mcd_img_catalog_create_final¶
Create Source Catalog from DetrendFinal.
1.5.12. mcd_img_catalog_create_illum¶
Create Source Catalog from DetrendIllum.
1.5.13. mcd_img_astrom_geom_correct¶
CorrectGeomDistortion.
TODO: describe
1.5.14. mcd_img_astrom_crossmatch¶
SpatialCrossmatch.
1.5.15. mcd_img_astrom_derive¶
DeriveAstrom.
1.5.16. mcd_img_catalog_create_astrom¶
Create Source Catalog using Astrometric solution.
1.5.17. mcd_img_photom_crossmatch¶
SpatialCrossmatch for photometric calibration.
1.5.18. mcd_img_photom_derive¶
DerivePhotom.
1.5.19. mcd_img_astrom_apply¶
ApplyAstrom.
1.5.20. mcd_img_photom_apply¶
ApplyPhotom.
1.5.21. mcd_img_stack_combine¶
None.
1.5.22. mcd_img_catalog_create_hci¶
Create Source Catalog from DetrendHCI.
1.5.23. mcd_img_hci_starpos_waffle_diffraction_extract¶
None.
1.5.24. mcd_img_hci_waffle_starpos_centroid¶
None.
1.5.25. mcd_img_hci_photom_compute¶
None.