0s autopkgtest [00:34:50]: starting date and time: 2024-03-26 00:34:50+0000 0s autopkgtest [00:34:50]: git checkout: 4a1cd702 l/adt_testbed: don't blame the testbed for unsolvable build deps 0s autopkgtest [00:34:50]: host juju-7f2275-prod-proposed-migration-environment-2; command line: /home/ubuntu/autopkgtest/runner/autopkgtest --output-dir /tmp/autopkgtest-work.owiokrbw/out --timeout-copy=6000 --setup-commands /home/ubuntu/autopkgtest-cloud/worker-config-production/setup-canonical.sh --setup-commands /home/ubuntu/autopkgtest/setup-commands/setup-testbed --apt-pocket=proposed --apt-upgrade cpl-plugin-muse --timeout-short=300 --timeout-copy=20000 --timeout-build=20000 '--env=ADT_TEST_TRIGGERS=astropy/6.0.0-1ubuntu1 cpl/7.3.2+ds-1build2 sphinx/7.2.6-6 wget/1.21.4-1ubuntu2' -- ssh -s /home/ubuntu/autopkgtest/ssh-setup/nova -- --flavor autopkgtest --security-groups autopkgtest-juju-7f2275-prod-proposed-migration-environment-2@lcy02-47.secgroup --name adt-noble-amd64-cpl-plugin-muse-20240326-003449-juju-7f2275-prod-proposed-migration-environment-2 --image adt/ubuntu-noble-amd64-server --keyname testbed-juju-7f2275-prod-proposed-migration-environment-2 --net-id=net_prod-proposed-migration -e TERM=linux -e ''"'"'http_proxy=http://squid.internal:3128'"'"'' -e ''"'"'https_proxy=http://squid.internal:3128'"'"'' -e ''"'"'no_proxy=127.0.0.1,127.0.1.1,login.ubuntu.com,localhost,localdomain,novalocal,internal,archive.ubuntu.com,ports.ubuntu.com,security.ubuntu.com,ddebs.ubuntu.com,changelogs.ubuntu.com,launchpadlibrarian.net,launchpadcontent.net,launchpad.net,10.24.0.0/24,keystone.ps5.canonical.com,objectstorage.prodstack5.canonical.com'"'"'' --mirror=http://ftpmaster.internal/ubuntu/ 66s autopkgtest [00:35:56]: testbed dpkg architecture: amd64 67s autopkgtest [00:35:57]: testbed apt version: 2.7.12 67s autopkgtest [00:35:57]: @@@@@@@@@@@@@@@@@@@@ test bed setup 67s Get:1 http://ftpmaster.internal/ubuntu noble-proposed InRelease [117 kB] 67s Get:2 http://ftpmaster.internal/ubuntu noble-proposed/restricted Sources [7592 B] 67s Get:3 http://ftpmaster.internal/ubuntu noble-proposed/main Sources [497 kB] 67s Get:4 http://ftpmaster.internal/ubuntu noble-proposed/multiverse Sources [56.0 kB] 67s Get:5 http://ftpmaster.internal/ubuntu noble-proposed/universe Sources [3976 kB] 67s Get:6 http://ftpmaster.internal/ubuntu noble-proposed/main i386 Packages [484 kB] 67s Get:7 http://ftpmaster.internal/ubuntu noble-proposed/main amd64 Packages [731 kB] 67s Get:8 http://ftpmaster.internal/ubuntu noble-proposed/main amd64 c-n-f Metadata [3508 B] 67s Get:9 http://ftpmaster.internal/ubuntu noble-proposed/restricted i386 Packages [6700 B] 67s Get:10 http://ftpmaster.internal/ubuntu noble-proposed/restricted amd64 Packages [37.9 kB] 67s Get:11 http://ftpmaster.internal/ubuntu noble-proposed/restricted amd64 c-n-f Metadata [116 B] 67s Get:12 http://ftpmaster.internal/ubuntu noble-proposed/universe amd64 Packages [4390 kB] 67s Get:13 http://ftpmaster.internal/ubuntu noble-proposed/universe i386 Packages [1260 kB] 67s Get:14 http://ftpmaster.internal/ubuntu noble-proposed/universe amd64 c-n-f Metadata [9396 B] 67s Get:15 http://ftpmaster.internal/ubuntu noble-proposed/multiverse i386 Packages [28.6 kB] 67s Get:16 http://ftpmaster.internal/ubuntu noble-proposed/multiverse amd64 Packages [96.8 kB] 67s Get:17 http://ftpmaster.internal/ubuntu noble-proposed/multiverse amd64 c-n-f Metadata [196 B] 70s Fetched 11.7 MB in 2s (7418 kB/s) 71s Reading package lists... 72s Reading package lists... 73s Building dependency tree... 73s Reading state information... 73s Calculating upgrade... 73s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 73s Reading package lists... 74s Building dependency tree... 74s Reading state information... 74s 0 upgraded, 0 newly installed, 0 to remove and 248 not upgraded. 74s sh: Attempting to set up Debian/Ubuntu apt sources automatically 74s sh: Distribution appears to be Ubuntu 75s Reading package lists... 76s Building dependency tree... 76s Reading state information... 76s eatmydata is already the newest version (131-1). 76s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 76s Reading package lists... 76s Building dependency tree... 76s Reading state information... 77s dbus is already the newest version (1.14.10-4ubuntu1). 77s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 77s Reading package lists... 77s Building dependency tree... 77s Reading state information... 77s rng-tools-debian is already the newest version (2.4). 77s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 78s Reading package lists... 78s Building dependency tree... 78s Reading state information... 78s The following packages will be REMOVED: 78s cloud-init* python3-configobj* python3-debconf* 78s 0 upgraded, 0 newly installed, 3 to remove and 0 not upgraded. 78s After this operation, 3256 kB disk space will be freed. 79s (Reading database ... (Reading database ... 5% (Reading database ... 10% (Reading database ... 15% (Reading database ... 20% (Reading database ... 25% (Reading database ... 30% (Reading database ... 35% (Reading database ... 40% (Reading database ... 45% (Reading database ... 50% (Reading database ... 55% (Reading database ... 60% (Reading database ... 65% (Reading database ... 70% (Reading database ... 75% (Reading database ... 80% (Reading database ... 85% (Reading database ... 90% (Reading database ... 95% (Reading database ... 100% (Reading database ... 71864 files and directories currently installed.) 79s Removing cloud-init (24.1.2-0ubuntu1) ... 79s Removing python3-configobj (5.0.8-3) ... 79s Removing python3-debconf (1.5.86) ... 79s Processing triggers for man-db (2.12.0-3) ... 80s (Reading database ... (Reading database ... 5% (Reading database ... 10% (Reading database ... 15% (Reading database ... 20% (Reading database ... 25% (Reading database ... 30% (Reading database ... 35% (Reading database ... 40% (Reading database ... 45% (Reading database ... 50% (Reading database ... 55% (Reading database ... 60% (Reading database ... 65% (Reading database ... 70% (Reading database ... 75% (Reading database ... 80% (Reading database ... 85% (Reading database ... 90% (Reading database ... 95% (Reading database ... 100% (Reading database ... 71475 files and directories currently installed.) 80s Purging configuration files for cloud-init (24.1.2-0ubuntu1) ... 81s dpkg: warning: while removing cloud-init, directory '/etc/cloud/cloud.cfg.d' not empty so not removed 81s Processing triggers for rsyslog (8.2312.0-3ubuntu3) ... 81s invoke-rc.d: policy-rc.d denied execution of try-restart. 81s Reading package lists... 81s Building dependency tree... 81s Reading state information... 82s linux-generic is already the newest version (6.8.0-11.11+1). 82s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 82s Hit:1 http://ftpmaster.internal/ubuntu noble InRelease 82s Hit:2 http://ftpmaster.internal/ubuntu noble-updates InRelease 82s Hit:3 http://ftpmaster.internal/ubuntu noble-security InRelease 84s Reading package lists... 84s Reading package lists... 84s Building dependency tree... 84s Reading state information... 85s Calculating upgrade... 85s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 85s Reading package lists... 85s Building dependency tree... 85s Reading state information... 86s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 86s autopkgtest [00:36:16]: rebooting testbed after setup commands that affected boot 113s autopkgtest [00:36:43]: testbed running kernel: Linux 6.8.0-11-generic #11-Ubuntu SMP PREEMPT_DYNAMIC Wed Feb 14 00:29:05 UTC 2024 114s autopkgtest [00:36:44]: @@@@@@@@@@@@@@@@@@@@ apt-source cpl-plugin-muse 116s Get:1 http://ftpmaster.internal/ubuntu noble/universe cpl-plugin-muse 2.8.7+dfsg-3 (dsc) [2420 B] 116s Get:2 http://ftpmaster.internal/ubuntu noble/universe cpl-plugin-muse 2.8.7+dfsg-3 (tar) [1586 kB] 116s Get:3 http://ftpmaster.internal/ubuntu noble/universe cpl-plugin-muse 2.8.7+dfsg-3 (diff) [14.6 kB] 116s gpgv: Signature made Tue Aug 16 06:12:08 2022 UTC 116s gpgv: using RSA key BAFC6C85F7CB143FEEB6FB157115AFD07710DCF7 116s gpgv: Can't check signature: No public key 116s dpkg-source: warning: cannot verify inline signature for ./cpl-plugin-muse_2.8.7+dfsg-3.dsc: no acceptable signature found 116s autopkgtest [00:36:46]: testing package cpl-plugin-muse version 2.8.7+dfsg-3 116s autopkgtest [00:36:46]: build not needed 116s autopkgtest [00:36:46]: test test-recipe.py: preparing testbed 117s Reading package lists... 117s Building dependency tree... 117s Reading state information... 118s Starting pkgProblemResolver with broken count: 0 118s Starting 2 pkgProblemResolver with broken count: 0 118s Done 118s The following additional packages will be installed: 118s cpl-plugin-muse libblas3 libcext0 libcfitsio10 libcplcore26 libcpldfs26 118s libcpldrs26 libcplui26 liberfa1 libfftw3-double3 libfftw3-single3 118s libgfortran5 libgomp1 libgsl27 libgslcblas0 libjs-jquery 118s libjs-jquery-hotkeys libjs-jquery-isonscreen libjs-jquery-metadata 118s libjs-jquery-tablesorter libjs-jquery-throttle-debounce libjs-sphinxdoc 118s libjs-underscore liblapack3 libwcs8 python3-astropy 118s python3-astropy-iers-data python3-configobj python3-coverage python3-cpl 118s python3-dateutil python3-erfa python3-hypothesis python3-iniconfig 118s python3-numpy python3-packaging python3-pluggy python3-ply python3-pytest 118s python3-pytest-arraydiff python3-pytest-astropy 118s python3-pytest-astropy-header python3-pytest-cov python3-pytest-doctestplus 118s python3-pytest-filter-subpackage python3-pytest-mock 118s python3-pytest-remotedata python3-sortedcontainers 118s Suggested packages: 118s cpl-plugin-muse-calib cpl-plugin-muse-doc libfftw3-bin libfftw3-dev 118s gsl-ref-psdoc | gsl-doc-pdf | gsl-doc-info | gsl-ref-html libxml2-utils 118s python-astropy-doc python3-astropy-affiliated python3-bs4 python3-h5py 118s python3-matplotlib python3-pandas python-configobj-doc python-coverage-doc 118s gdb python-hypothesis-doc gcc gfortran python3-dev python-ply-doc 118s python-pytest-mock-doc python-sortedcontainers-doc 118s Recommended packages: 118s javascript-common libjs-jquery-datatables python3-scipy python3-click 118s The following NEW packages will be installed: 118s autopkgtest-satdep cpl-plugin-muse libblas3 libcext0 libcfitsio10 118s libcplcore26 libcpldfs26 libcpldrs26 libcplui26 liberfa1 libfftw3-double3 118s libfftw3-single3 libgfortran5 libgomp1 libgsl27 libgslcblas0 libjs-jquery 118s libjs-jquery-hotkeys libjs-jquery-isonscreen libjs-jquery-metadata 118s libjs-jquery-tablesorter libjs-jquery-throttle-debounce libjs-sphinxdoc 118s libjs-underscore liblapack3 libwcs8 python3-astropy 118s python3-astropy-iers-data python3-configobj python3-coverage python3-cpl 118s python3-dateutil python3-erfa python3-hypothesis python3-iniconfig 118s python3-numpy python3-packaging python3-pluggy python3-ply python3-pytest 118s python3-pytest-arraydiff python3-pytest-astropy 118s python3-pytest-astropy-header python3-pytest-cov python3-pytest-doctestplus 118s python3-pytest-filter-subpackage python3-pytest-mock 118s python3-pytest-remotedata python3-sortedcontainers 118s 0 upgraded, 49 newly installed, 0 to remove and 0 not upgraded. 118s Need to get 25.8 MB/25.8 MB of archives. 118s After this operation, 116 MB of additional disk space will be used. 118s Get:1 /tmp/autopkgtest.6NTcjL/1-autopkgtest-satdep.deb autopkgtest-satdep amd64 0 [724 B] 118s Get:2 http://ftpmaster.internal/ubuntu noble/main amd64 libjs-jquery all 3.6.1+dfsg+~3.5.14-1 [328 kB] 118s Get:3 http://ftpmaster.internal/ubuntu noble/universe amd64 libjs-jquery-hotkeys all 0~20130707+git2d51e3a9+dfsg-2ubuntu2 [11.5 kB] 118s Get:4 http://ftpmaster.internal/ubuntu noble/universe amd64 libcext0 amd64 7.3.2+ds-1build1 [32.2 kB] 118s Get:5 http://ftpmaster.internal/ubuntu noble/universe amd64 libcfitsio10 amd64 4.3.1-1 [528 kB] 118s Get:6 http://ftpmaster.internal/ubuntu noble/main amd64 libgomp1 amd64 14-20240303-1ubuntu1 [147 kB] 118s Get:7 http://ftpmaster.internal/ubuntu noble/main amd64 libfftw3-double3 amd64 3.3.10-1ubuntu1 [835 kB] 118s Get:8 http://ftpmaster.internal/ubuntu noble/main amd64 libfftw3-single3 amd64 3.3.10-1ubuntu1 [869 kB] 118s Get:9 http://ftpmaster.internal/ubuntu noble/universe amd64 libcplcore26 amd64 7.3.2+ds-1build1 [489 kB] 118s Get:10 http://ftpmaster.internal/ubuntu noble/universe amd64 libcplui26 amd64 7.3.2+ds-1build1 [39.3 kB] 118s Get:11 http://ftpmaster.internal/ubuntu noble/universe amd64 libcpldfs26 amd64 7.3.2+ds-1build1 [41.1 kB] 118s Get:12 http://ftpmaster.internal/ubuntu noble/universe amd64 libwcs8 amd64 8.2.2+ds-3 [310 kB] 118s Get:13 http://ftpmaster.internal/ubuntu noble/universe amd64 libcpldrs26 amd64 7.3.2+ds-1build1 [67.2 kB] 118s Get:14 http://ftpmaster.internal/ubuntu noble/universe amd64 libgslcblas0 amd64 2.7.1+dfsg-6ubuntu1 [104 kB] 118s Get:15 http://ftpmaster.internal/ubuntu noble/universe amd64 libgsl27 amd64 2.7.1+dfsg-6ubuntu1 [987 kB] 118s Get:16 http://ftpmaster.internal/ubuntu noble/universe amd64 cpl-plugin-muse amd64 2.8.7+dfsg-3 [540 kB] 118s Get:17 http://ftpmaster.internal/ubuntu noble/main amd64 libblas3 amd64 3.12.0-3 [238 kB] 118s Get:18 http://ftpmaster.internal/ubuntu noble/main amd64 libgfortran5 amd64 14-20240303-1ubuntu1 [924 kB] 119s Get:19 http://ftpmaster.internal/ubuntu noble/universe amd64 libjs-jquery-metadata all 12-4 [6582 B] 119s Get:20 http://ftpmaster.internal/ubuntu noble/universe amd64 libjs-jquery-tablesorter all 1:2.31.3+dfsg1-3 [193 kB] 119s Get:21 http://ftpmaster.internal/ubuntu noble/universe amd64 libjs-jquery-throttle-debounce all 1.1+dfsg.1-2 [12.5 kB] 119s Get:22 http://ftpmaster.internal/ubuntu noble/main amd64 libjs-underscore all 1.13.4~dfsg+~1.11.4-3 [118 kB] 119s Get:23 http://ftpmaster.internal/ubuntu noble/main amd64 libjs-sphinxdoc all 7.2.6-4 [149 kB] 119s Get:24 http://ftpmaster.internal/ubuntu noble/main amd64 liblapack3 amd64 3.12.0-3 [2649 kB] 119s Get:25 http://ftpmaster.internal/ubuntu noble/main amd64 python3-configobj all 5.0.8-3 [33.8 kB] 119s Get:26 http://ftpmaster.internal/ubuntu noble/universe amd64 python3-iniconfig all 1.1.1-2 [6024 B] 119s Get:27 http://ftpmaster.internal/ubuntu noble/main amd64 python3-packaging all 23.2-1 [40.6 kB] 119s Get:28 http://ftpmaster.internal/ubuntu noble/universe amd64 python3-pluggy all 1.4.0-1 [20.4 kB] 119s Get:29 http://ftpmaster.internal/ubuntu noble/universe amd64 python3-pytest all 7.4.4-1 [305 kB] 119s Get:30 http://ftpmaster.internal/ubuntu noble/main amd64 python3-dateutil all 2.8.2-3 [79.2 kB] 119s Get:31 http://ftpmaster.internal/ubuntu noble/main amd64 python3-sortedcontainers all 2.4.0-2 [27.6 kB] 119s Get:32 http://ftpmaster.internal/ubuntu noble/universe amd64 python3-hypothesis all 6.92.2-1 [371 kB] 119s Get:33 http://ftpmaster.internal/ubuntu noble/main amd64 python3-numpy amd64 1:1.24.2-2 [7141 kB] 119s Get:34 http://ftpmaster.internal/ubuntu noble/universe amd64 python3-pytest-arraydiff all 0.6.1-2 [10.2 kB] 119s Get:35 http://ftpmaster.internal/ubuntu noble/universe amd64 python3-pytest-astropy-header all 0.2.2-1 [8190 B] 119s Get:36 http://ftpmaster.internal/ubuntu noble/universe amd64 python3-coverage amd64 7.3.2-0ubuntu1 [146 kB] 119s Get:37 http://ftpmaster.internal/ubuntu noble/universe amd64 libjs-jquery-isonscreen all 1.2.0-1.1 [3244 B] 119s Get:38 http://ftpmaster.internal/ubuntu noble/universe amd64 python3-pytest-cov all 4.1.0-1 [21.5 kB] 119s Get:39 http://ftpmaster.internal/ubuntu noble/universe amd64 python3-pytest-doctestplus all 1.2.0-1 [23.1 kB] 119s Get:40 http://ftpmaster.internal/ubuntu noble/universe amd64 python3-pytest-filter-subpackage all 0.2.0-1 [6094 B] 119s Get:41 http://ftpmaster.internal/ubuntu noble/universe amd64 python3-pytest-mock all 3.12.0-1.1 [11.3 kB] 119s Get:42 http://ftpmaster.internal/ubuntu noble/universe amd64 python3-pytest-remotedata all 0.4.1-1 [8650 B] 119s Get:43 http://ftpmaster.internal/ubuntu noble/universe amd64 python3-pytest-astropy all 0.11.0-1 [5902 B] 119s Get:44 http://ftpmaster.internal/ubuntu noble/main amd64 python3-ply all 3.11-6 [46.5 kB] 119s Get:45 http://ftpmaster.internal/ubuntu noble/universe amd64 python3-astropy-iers-data all 0.2024.01.01.00.33.39-1 [2046 kB] 119s Get:46 http://ftpmaster.internal/ubuntu noble/universe amd64 liberfa1 amd64 2.0.1-1 [139 kB] 119s Get:47 http://ftpmaster.internal/ubuntu noble/universe amd64 python3-erfa amd64 2.0.1.1+ds-3 [313 kB] 119s Get:48 http://ftpmaster.internal/ubuntu noble/universe amd64 python3-astropy amd64 6.0.0-1 [5335 kB] 119s Get:49 http://ftpmaster.internal/ubuntu noble/universe amd64 python3-cpl amd64 0.7.4-2build9 [37.1 kB] 119s Fetched 25.8 MB in 0s (52.6 MB/s) 119s Selecting previously unselected package libjs-jquery. 120s (Reading database ... (Reading database ... 5% (Reading database ... 10% (Reading database ... 15% (Reading database ... 20% (Reading database ... 25% (Reading database ... 30% (Reading database ... 35% (Reading database ... 40% (Reading database ... 45% (Reading database ... 50% (Reading database ... 55% (Reading database ... 60% (Reading database ... 65% (Reading database ... 70% (Reading database ... 75% (Reading database ... 80% (Reading database ... 85% (Reading database ... 90% (Reading database ... 95% (Reading database ... 100% (Reading database ... 71420 files and directories currently installed.) 120s Preparing to unpack .../00-libjs-jquery_3.6.1+dfsg+~3.5.14-1_all.deb ... 120s Unpacking libjs-jquery (3.6.1+dfsg+~3.5.14-1) ... 120s Selecting previously unselected package libjs-jquery-hotkeys. 120s Preparing to unpack .../01-libjs-jquery-hotkeys_0~20130707+git2d51e3a9+dfsg-2ubuntu2_all.deb ... 120s Unpacking libjs-jquery-hotkeys (0~20130707+git2d51e3a9+dfsg-2ubuntu2) ... 120s Selecting previously unselected package libcext0:amd64. 120s Preparing to unpack .../02-libcext0_7.3.2+ds-1build1_amd64.deb ... 120s Unpacking libcext0:amd64 (7.3.2+ds-1build1) ... 120s Selecting previously unselected package libcfitsio10:amd64. 120s Preparing to unpack .../03-libcfitsio10_4.3.1-1_amd64.deb ... 120s Unpacking libcfitsio10:amd64 (4.3.1-1) ... 120s Selecting previously unselected package libgomp1:amd64. 120s Preparing to unpack .../04-libgomp1_14-20240303-1ubuntu1_amd64.deb ... 120s Unpacking libgomp1:amd64 (14-20240303-1ubuntu1) ... 120s Selecting previously unselected package libfftw3-double3:amd64. 120s Preparing to unpack .../05-libfftw3-double3_3.3.10-1ubuntu1_amd64.deb ... 120s Unpacking libfftw3-double3:amd64 (3.3.10-1ubuntu1) ... 120s Selecting previously unselected package libfftw3-single3:amd64. 120s Preparing to unpack .../06-libfftw3-single3_3.3.10-1ubuntu1_amd64.deb ... 120s Unpacking libfftw3-single3:amd64 (3.3.10-1ubuntu1) ... 120s Selecting previously unselected package libcplcore26:amd64. 120s Preparing to unpack .../07-libcplcore26_7.3.2+ds-1build1_amd64.deb ... 120s Unpacking libcplcore26:amd64 (7.3.2+ds-1build1) ... 120s Selecting previously unselected package libcplui26:amd64. 120s Preparing to unpack .../08-libcplui26_7.3.2+ds-1build1_amd64.deb ... 120s Unpacking libcplui26:amd64 (7.3.2+ds-1build1) ... 120s Selecting previously unselected package libcpldfs26:amd64. 120s Preparing to unpack .../09-libcpldfs26_7.3.2+ds-1build1_amd64.deb ... 120s Unpacking libcpldfs26:amd64 (7.3.2+ds-1build1) ... 120s Selecting previously unselected package libwcs8:amd64. 120s Preparing to unpack .../10-libwcs8_8.2.2+ds-3_amd64.deb ... 120s Unpacking libwcs8:amd64 (8.2.2+ds-3) ... 120s Selecting previously unselected package libcpldrs26:amd64. 120s Preparing to unpack .../11-libcpldrs26_7.3.2+ds-1build1_amd64.deb ... 120s Unpacking libcpldrs26:amd64 (7.3.2+ds-1build1) ... 120s Selecting previously unselected package libgslcblas0:amd64. 120s Preparing to unpack .../12-libgslcblas0_2.7.1+dfsg-6ubuntu1_amd64.deb ... 120s Unpacking libgslcblas0:amd64 (2.7.1+dfsg-6ubuntu1) ... 120s Selecting previously unselected package libgsl27:amd64. 120s Preparing to unpack .../13-libgsl27_2.7.1+dfsg-6ubuntu1_amd64.deb ... 120s Unpacking libgsl27:amd64 (2.7.1+dfsg-6ubuntu1) ... 120s Selecting previously unselected package cpl-plugin-muse:amd64. 120s Preparing to unpack .../14-cpl-plugin-muse_2.8.7+dfsg-3_amd64.deb ... 120s Unpacking cpl-plugin-muse:amd64 (2.8.7+dfsg-3) ... 120s Selecting previously unselected package libblas3:amd64. 120s Preparing to unpack .../15-libblas3_3.12.0-3_amd64.deb ... 120s Unpacking libblas3:amd64 (3.12.0-3) ... 120s Selecting previously unselected package libgfortran5:amd64. 120s Preparing to unpack .../16-libgfortran5_14-20240303-1ubuntu1_amd64.deb ... 120s Unpacking libgfortran5:amd64 (14-20240303-1ubuntu1) ... 120s Selecting previously unselected package libjs-jquery-metadata. 120s Preparing to unpack .../17-libjs-jquery-metadata_12-4_all.deb ... 120s Unpacking libjs-jquery-metadata (12-4) ... 120s Selecting previously unselected package libjs-jquery-tablesorter. 120s Preparing to unpack .../18-libjs-jquery-tablesorter_1%3a2.31.3+dfsg1-3_all.deb ... 120s Unpacking libjs-jquery-tablesorter (1:2.31.3+dfsg1-3) ... 121s Selecting previously unselected package libjs-jquery-throttle-debounce. 121s Preparing to unpack .../19-libjs-jquery-throttle-debounce_1.1+dfsg.1-2_all.deb ... 121s Unpacking libjs-jquery-throttle-debounce (1.1+dfsg.1-2) ... 121s Selecting previously unselected package libjs-underscore. 121s Preparing to unpack .../20-libjs-underscore_1.13.4~dfsg+~1.11.4-3_all.deb ... 121s Unpacking libjs-underscore (1.13.4~dfsg+~1.11.4-3) ... 121s Selecting previously unselected package libjs-sphinxdoc. 121s Preparing to unpack .../21-libjs-sphinxdoc_7.2.6-4_all.deb ... 121s Unpacking libjs-sphinxdoc (7.2.6-4) ... 121s Selecting previously unselected package liblapack3:amd64. 121s Preparing to unpack .../22-liblapack3_3.12.0-3_amd64.deb ... 121s Unpacking liblapack3:amd64 (3.12.0-3) ... 121s Selecting previously unselected package python3-configobj. 121s Preparing to unpack .../23-python3-configobj_5.0.8-3_all.deb ... 121s Unpacking python3-configobj (5.0.8-3) ... 121s Selecting previously unselected package python3-iniconfig. 121s Preparing to unpack .../24-python3-iniconfig_1.1.1-2_all.deb ... 121s Unpacking python3-iniconfig (1.1.1-2) ... 121s Selecting previously unselected package python3-packaging. 121s Preparing to unpack .../25-python3-packaging_23.2-1_all.deb ... 121s Unpacking python3-packaging (23.2-1) ... 121s Selecting previously unselected package python3-pluggy. 121s Preparing to unpack .../26-python3-pluggy_1.4.0-1_all.deb ... 121s Unpacking python3-pluggy (1.4.0-1) ... 121s Selecting previously unselected package python3-pytest. 121s Preparing to unpack .../27-python3-pytest_7.4.4-1_all.deb ... 121s Unpacking python3-pytest (7.4.4-1) ... 121s 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python3-cpl (0.7.4-2build9) ... 130s Setting up autopkgtest-satdep (0) ... 130s Processing triggers for man-db (2.12.0-3) ... 131s Processing triggers for libc-bin (2.39-0ubuntu6) ... 134s (Reading database ... 75465 files and directories currently installed.) 134s Removing autopkgtest-satdep (0) ... 134s autopkgtest [00:37:04]: test test-recipe.py: [----------------------- 134s Recipe muse_scibasic: 134s version 2.8.7 134s Parameters: {'nifu': 0, 'overscan': 'vpoly', 'ovscreject': 'dcr', 'ovscsigma': 30.0, 'ovscignore': 3, 'crop': True, 'cr': 'none', 'xbox': 15, 'ybox': 40, 'passes': 2, 'thres': 5.8, 'combine': 'none', 'nlow': 1, 'nhigh': 1, 'nkeep': 1, 'lsigma': 3.0, 'hsigma': 3.0, 'scale': True, 'saveimage': True, 'skylines': '5577.339,6300.304', 'skyhalfwidth': 5.0, 'skybinsize': 0.1, 'skyreject': '15.,15.,1', 'resample': False, 'dlambda': 1.25, 'merge': False} 134s Docstring: Remove the instrumental signature from the data of each CCD and 134s convert them from an image into a pixel table. 134s 134s Processing handles each raw input image separately: it trims the raw 134s data and records the overscan statistics, subtracts the bias (taking 134s account of the overscan, if --overscan is not "none"), optionally 134s detects cosmic rays (note that by default cosmic ray rejection is 134s handled in the post processing recipes while the data is reformatted 134s into a datacube, so that the default setting is cr="none" here), 134s converts the images from adu to count, subtracts the dark, divides by 134s the flat-field, and (optionally) propagates the integrated flux value 134s from the twilight-sky cube. The reduced image is then saved (if 134s --saveimage=true). The input calibrations geometry table, trace table, 134s and wavelength calibration table are used to assign 3D coordinates to 134s each CCD-based pixel, thereby creating a pixel table for each 134s exposure. If --skylines contains one or more wavelengths for (bright 134s and isolated) sky emission lines, these lines are used to correct the 134s wavelength calibration using an offset. The data is then cut to a 134s useful wavelength range (if --crop=true). If an ILLUM exposure was 134s given as input, it is then used to correct the relative illumination 134s between all slices of one IFU. For this, the data of each slice is 134s multiplied by the normalized median flux of that slice in the ILLUM 134s exposure. As last step, the data is divided by the normalized twilight 134s cube (if given), using the 3D coordinate of each pixel in the pixel 134s table to interpolate the twilight correction onto the data. This pre- 134s reduced pixel table for each exposure is then saved to disk. 134s 134s Parameters: 134s nifu: IFU to handle. If set to 0, all IFUs are processed 134s serially. If set to -1, all IFUs are processed in 134s parallel. (int; default: 0) 134s overscan: If this is "none", stop when detecting discrepant 134s overscan levels (see ovscsigma), for "offset" it 134s assumes that the mean overscan level represents the 134s real offset in the bias levels of the exposures 134s involved, and adjusts the data accordingly; for 134s "vpoly", a polynomial is fit to the vertical overscan 134s and subtracted from the whole quadrant. (str; default: 134s 'vpoly') 134s ovscreject: This influences how values are rejected when computing 134s overscan statistics. Either no rejection at all 134s ("none"), rejection using the DCR algorithm ("dcr"), or 134s rejection using an iterative constant fit ("fit"). 134s (str; default: 'dcr') 134s ovscsigma: If the deviation of mean overscan levels between a raw 134s input image and the reference image is higher than 134s |ovscsigma x stdev|, stop the processing. If 134s overscan="vpoly", this is used as sigma rejection level 134s for the iterative polynomial fit (the level comparison 134s is then done afterwards with |100 x stdev| to guard 134s against incompatible settings). Has no effect for 134s overscan="offset". (float; default: 30.0) 134s ovscignore: The number of pixels of the overscan adjacent to the 134s data section of the CCD that are ignored when computing 134s statistics or fits. (int; default: 3) 134s crop: Automatically crop the output pixel tables in 134s wavelength depending on the expected useful wavelength 134s range of the active instrument mode (4750-9350 Angstrom 134s for nominal mode and NFM, 4700-9350 Angstrom for 134s nominal AO mode, and 4600-9350 Angstrom for the 134s extended modes). (bool; default: True) 134s cr: Type of cosmic ray cleaning to use (for quick-look data 134s processing). (str; default: 'none') 134s xbox: Search box size in x. Only used if cr=dcr. (int; 134s default: 15) 134s ybox: Search box size in y. Only used if cr=dcr. (int; 134s default: 40) 134s passes: Maximum number of cleaning passes. Only used if cr=dcr. 134s (int; default: 2) 134s thres: Threshold for detection gap in factors of standard 134s deviation. Only used if cr=dcr. (float; default: 5.8) 134s combine: Type of combination to use. Note that in most cases, 134s science exposures cannot easily be combined on the CCD 134s level, so this should usually be kept as "none"! This 134s does not pay attention about the type of input data, 134s and will combine all raw inputs! (str; default: 'none') 134s nlow: Number of minimum pixels to reject with minmax (int; 134s default: 1) 134s nhigh: Number of maximum pixels to reject with minmax (int; 134s default: 1) 134s nkeep: Number of pixels to keep with minmax (int; default: 1) 134s lsigma: Low sigma for pixel rejection with sigclip (float; 134s default: 3.0) 134s hsigma: High sigma for pixel rejection with sigclip (float; 134s default: 3.0) 134s scale: Scale the individual images to a common exposure time 134s before combining them. (bool; default: True) 134s saveimage: Save the pre-processed CCD-based image of each input 134s exposure before it is transformed into a pixel table. 134s (bool; default: True) 134s skylines: List of wavelengths of sky emission lines (in Angstrom) 134s to use as reference for wavelength offset correction 134s using a Gaussian fit. It can contain multiple 134s (isolated) lines, as comma-separated list, individual 134s shifts are then combined into one weighted average 134s offset. Set to "none" to deactivate. (str; default: 134s '5577.339,6300.304') 134s skyhalfwidth: Half-width of the extraction box (in Angstrom) around 134s each sky emission line. (float; default: 5.0) 134s skybinsize: Size of the bins (in Angstrom per pixel) for the 134s intermediate spectrum to do the Gaussian fit to each 134s sky emission line. (float; default: 0.1) 134s skyreject: Sigma clipping parameters for the intermediate spectrum 134s to do the Gaussian fit to each sky emission line. Up to 134s three comma-separated numbers can be given, which are 134s interpreted as high sigma-clipping limit (float), low 134s limit (float), and number of iterations (integer), 134s respectively. (str; default: '15.,15.,1') 134s resample: Resample the input science data into 2D spectral images 134s using all supplied calibrations for a visual check. 134s Note that the image produced will show small wiggles 134s even when the input calibrations are good and were 134s applied successfully! (bool; default: False) 134s dlambda: Wavelength step (in Angstrom per pixel) to use for 134s resampling. (float; default: 1.25) 134s merge: Merge output products from different IFUs into a common 134s file. (bool; default: False) 134s 134s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 134s 'TRACE_TABLE', 'WAVECAL_TABLE', 'GEOMETRY_TABLE', 134s 'TWILIGHT_CUBE', 'BADPIX_TABLE'] 134s 134s Raw and product frames: 134s OBJECT --> ['OBJECT_RED', 'OBJECT_RESAMPLED', 'PIXTABLE_OBJECT'] 134s STD --> ['STD_RED', 'STD_RESAMPLED', 'PIXTABLE_STD'] 134s SKY --> ['SKY_RED', 'SKY_RESAMPLED', 'PIXTABLE_SKY'] 134s ASTROMETRY --> ['ASTROMETRY_RED', 'ASTROMETRY_RESAMPLED', 134s 'PIXTABLE_ASTROMETRY'] 134s ILLUM --> [] 134s REDUCED --> ['REDUCED_RESAMPLED', 'PIXTABLE_REDUCED'] 134s Author: Peter Weilbacher 134s 134s 134s Recipe muse_standard: 134s version 2.8.7 134s Parameters: {'profile': 'auto', 'select': 'distance', 'smooth': 'ppoly', 'lambdamin': 4000.0, 'lambdamax': 10000.0, 'lambdaref': 7000.0, 'darcheck': 'none', 'filter': 'white'} 134s Docstring: Create a flux response curve from a standard star exposure. 134s 134s Merge pixel tables from all IFUs and correct for differential 134s atmospheric refraction, when necessary. To derive the flux response 134s curve, integrate the flux of all objects detected within the field of 134s view using the given profile. Select one object as the standard star 134s (either the brightest or the one nearest one, depending on --select) 134s and compare its measured fluxes to tabulated fluxes to derive the 134s sensitivity over wavelength. Postprocess this sensitivity curve to 134s mark wavelength ranges affected by telluric absorption. Interpolate 134s over the telluric regions and derive a telluric correction spectrum 134s for them. The final response curve is then linearly extrapolated to 134s the largest possible MUSE wavelength range and smoothed (with the 134s method given by --smooth). The derivation of the telluric correction 134s spectrum assumes that the star has a smooth spectrum within the 134s telluric regions. If there are more than one exposure given in the 134s input data, the derivation of the flux response and telluric 134s corrections are done separately for each exposure. For each exposure, 134s an image containing the extracted stellar spectra and the datacube 134s used for flux integration are saved, together with collapsed images 134s for each given filter. In MUSE's WFM data (both AO and non-AO), the 134s Moffat profile is a good approximation of the actual PSF. Using the 134s smoothed profile ("smoffat") helps to increase the S/N and in most 134s cases removes systematics. In NFM, however, the profile is a 134s combination of a wide PSF plus the central AO-corrected peak, which 134s cannot be fit well by an analytical profile. In this case the circular 134s aperture is the best way to extract the flux. Using --profile="auto" 134s (the default) selects these options to give the best flux extraction 134s for most cases. 134s 134s Parameters: 134s profile: Type of flux integration to use. "gaussian", "moffat", and 134s "smoffat" use 2D profile fitting, "circle" and "square" 134s are non-optimal aperture flux integrators. "smoffat" uses 134s smoothing of the Moffat parameters from an initial fit, to 134s derive physically meaningful wavelength- dependent 134s behavior. "auto" selects the smoothed Moffat profile for 134s WFM data and circular flux integration for NFM. (str; 134s default: 'auto') 134s select: How to select the star for flux integration, "flux" uses 134s the brightest star in the field, "distance" uses the 134s detection nearest to the approximate coordinates of the 134s reference source. (str; default: 'distance') 134s smooth: How to smooth the response curve before writing it to 134s disk. "none" does not do any kind of smoothing (such a 134s response curve is only useful, if smoothed externally; 134s "median" does a median-filter of 15 Angstrom half-width; 134s "ppoly" fits piecewise cubic polynomials (each one across 134s 2x150 Angstrom width) postprocessed by a sliding average 134s filter of 15 Angstrom half-width. (str; default: 'ppoly') 134s lambdamin: Cut off the data below this wavelength after loading the 134s pixel table(s). (float; default: 4000.0) 134s lambdamax: Cut off the data above this wavelength after loading the 134s pixel table(s). (float; default: 10000.0) 134s lambdaref: Reference wavelength used for correction of differential 134s atmospheric refraction. The R-band (peak wavelength ~7000 134s Angstrom) that is usually used for guiding, is close to 134s the central wavelength of MUSE, so a value of 7000.0 134s Angstrom should be used if nothing else is known. A value 134s less than zero switches DAR correction off. (float; 134s default: 7000.0) 134s darcheck: Carry out a check of the theoretical DAR correction using 134s source centroiding. If "correct" it will also apply an 134s empirical correction. (str; default: 'none') 134s filter: The filter name(s) to be used for the output field-of-view 134s image. Each name has to correspond to an EXTNAME in an 134s extension of the FILTER_LIST file. If an unsupported 134s filter name is given, creation of the respective image is 134s omitted. If multiple filter names are given, they have to 134s be comma separated. If the zeropoint QC parameters are 134s wanted, make sure to add "Johnson_V,Cousins_R,Cousins_I". 134s (str; default: 'white') 134s 134s Calibration frames: ['EXTINCT_TABLE', 'STD_FLUX_TABLE', 134s 'TELLURIC_REGIONS', 'FILTER_LIST'] 134s 134s Raw and product frames: 134s PIXTABLE_STD --> ['DATACUBE_STD', 'STD_FLUXES', 'STD_RESPONSE', 134s 'STD_TELLURIC'] 134s Author: Peter Weilbacher 134s 134s 134s Recipe muse_exp_align: 134s version 2.8.7 134s Parameters: {'rsearch': '30.,4.,2.,0.8', 'nbins': 60, 'weight': True, 'fwhm': 5.0, 'threshold': 15.0, 'bkgignore': 0.05, 'bkgfraction': 0.1, 'step': 0.5, 'iterations': 100000, 'srcmin': 5, 'srcmax': 80, 'roundmin': -1.0, 'roundmax': 1.0, 'sharpmin': 0.2, 'sharpmax': 1.0, 'expmap': False, 'bpixdistance': 5.0, 'override_detection': False} 134s Docstring: Create a coordinate offset table to be used to align exposures during 134s exposure combination. 134s 134s Compute the coordinate offset for each input field-of-view image with 134s respect to a reference. The created list of coordinate offsets can 134s then be used in muse_exp_combine as the field coordinate offsets to 134s properly align the exposures during their combination. The source 134s positions used to compute the field offsets are obtained by detecting 134s point sources in each of the input images, unless the source detection 134s is overridden and an input source list is available for each input 134s field-of-view image. In this latter case the input source positions 134s are used to calculate the field offsets. 134s 134s Parameters: 134s rsearch: Search radius (in arcsec) for each iteration of 134s the offset computation. (str; default: 134s '30.,4.,2.,0.8') 134s nbins: Number of bins to use for 2D histogram on the 134s first iteration of the offset computation. (int; 134s default: 60) 134s weight: Use weighting. (bool; default: True) 134s fwhm: FWHM in pixels of the convolution filter. (float; 134s default: 5.0) 134s threshold: Initial intensity threshold for detecting point 134s sources. If the value is negative or zero the 134s threshold is taken as sigma above median 134s background MAD. If it is larger than zero the 134s threshold is taken as absolute background level. 134s (float; default: 15.0) 134s bkgignore: Fraction of the image to be ignored. (float; 134s default: 0.05) 134s bkgfraction: Fraction of the image (without the ignored part) 134s to be considered as background. (float; default: 134s 0.1) 134s step: Increment/decrement of the threshold value in 134s subsequent iterations. (float; default: 0.5) 134s iterations: Maximum number of iterations used for detecting 134s sources. (int; default: 100000) 134s srcmin: Minimum number of sources which must be found. 134s (int; default: 5) 134s srcmax: Maximum number of sources which may be found. 134s (int; default: 80) 134s roundmin: Lower limit of the allowed point-source 134s roundness. (float; default: -1.0) 134s roundmax: Upper limit of the allowed point-source 134s roundness. (float; default: 1.0) 134s sharpmin: Lower limit of the allowed point-source 134s sharpness. (float; default: 0.2) 134s sharpmax: Upper limit of the allowed point-source 134s sharpness. (float; default: 1.0) 134s expmap: Enables the creation of a simple exposure map for 134s the combined field- of-view. (bool; default: 134s False) 134s bpixdistance: Minimum allowed distance of a source to the 134s closest bad pixel in pixel. Detected sources 134s which are closer to a bad pixel are not taken 134s into account when computing the field offsets. 134s This option has no effect if the source positions 134s are taken from input catalogs. (float; default: 134s 5.0) 134s override_detection: Overrides the source detection step. If this is 134s enabled and source catalogs are present in the 134s input data set, the source positions used to 134s calculate the field offsets are read from the 134s input catalogs. If no catalogs are available as 134s input data the source positions are detected on 134s the input images. (bool; default: False) 134s 134s Calibration frames: ['SOURCE_LIST'] 134s 134s Raw and product frames: 134s IMAGE_FOV --> ['EXPOSURE_MAP', 'PREVIEW_FOV', 'SOURCE_LIST', 134s 'OFFSET_LIST'] 134s Author: Ralf Palsa 134s 134s 134s Recipe muse_scipost_correct_dar: 134s version 2.8.7 134s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'lambdaref': 7000.0, 'darcheck': 'none'} 134s Docstring: Apply DAR correction for MUSE pixel tables. 134s 134s Correct the coordinates in the pixel table by differential atmospheric 134s refraction. This is a task separated from muse_scipost. 134s 134s Parameters: 134s lambdamin: Cut off the data below this wavelength after loading the 134s pixel table(s). (float; default: 4000.0) 134s lambdamax: Cut off the data above this wavelength after loading the 134s pixel table(s). (float; default: 10000.0) 134s lambdaref: Reference wavelength used for correction of differential 134s atmospheric refraction. The R-band (peak wavelength ~7000 134s Angstrom) that is usually used for guiding, is close to 134s the central wavelength of MUSE, so a value of 7000.0 134s Angstrom should be used if nothing else is known. A value 134s less than zero switches DAR correction off. (float; 134s default: 7000.0) 134s darcheck: Carry out a check of the theoretical DAR correction using 134s source centroiding. If "correct" it will also apply an 134s empirical correction. (str; default: 'none') 134s 134s Calibration frames: [] 134s 134s Raw and product frames: 134s PIXTABLE_OBJECT --> ['PIXTABLE_OBJECT'] 134s Author: Ole Streicher 134s 134s 134s Recipe muse_scipost_correct_rv: 134s version 2.8.7 134s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'rvcorr': 'bary'} 134s Docstring: Apply RV correction for MUSE pixel tables. 134s 134s Correct the wavelengths in the pixel table by given radial-velocity 134s correction. This is a task separated from muse_scipost. 134s 134s Parameters: 134s lambdamin: Cut off the data below this wavelength after loading the 134s pixel table(s). (float; default: 4000.0) 134s lambdamax: Cut off the data above this wavelength after loading the 134s pixel table(s). (float; default: 10000.0) 134s rvcorr: Correct the radial velocity of the telescope with 134s reference to either the barycenter of the Solar System 134s (bary), the center of the Sun (helio), or to the center of 134s the Earth (geo). (str; default: 'bary') 134s 134s Calibration frames: [] 134s 134s Raw and product frames: 134s PIXTABLE_OBJECT --> ['PIXTABLE_REDUCED'] 134s Author: Peter Weilbacher 134s 134s 134s Recipe muse_scipost_subtract_sky_simple: 134s version 2.8.7 134s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0} 134s Docstring: Subtract night sky spectrum. 134s 134s Subtract the sky in a simple way, just using a sky spectrum created by 134s muse_create_sky. This is a separated task of muse_scipost. 134s 134s Parameters: 134s lambdamin: Cut off the data below this wavelength after loading the 134s pixel table(s). (float; default: 4000.0) 134s lambdamax: Cut off the data above this wavelength after loading the 134s pixel table(s). (float; default: 10000.0) 134s 134s Calibration frames: ['SKY_SPECTRUM'] 134s 134s Raw and product frames: 134s PIXTABLE_REDUCED --> ['PIXTABLE_REDUCED'] 134s Author: Peter Weilbacher 134s 134s 134s Recipe muse_geometry: 134s version 2.8.7 134s Parameters: {'ifu1': 1, 'ifu2': 24, 'sigma': 2.2, 'centroid': 'gaussian', 'smooth': 1.5, 'lambdamin': 6800.0, 'lambdamax': 7200.0} 134s Docstring: Compute relative location of the slices within the field of view and 134s measure the instrumental PSF on the detectors. 134s 134s Processing first works separately on each IFU of the raw input data 134s (in parallel): it trims the raw data and records the overscan 134s statistics, subtracts the bias and converts them from adu to count. 134s Optionally, the dark can be subtracted and the data can be divided by 134s the flat-field. The data of all input mask exposures is then averaged. 134s The averaged image together with the trace table and wavelength 134s calibration as well as the line catalog are used to detect spots. The 134s detection windows are used to measure the spots on all images of the 134s sequence, the result is saved, with information on the measured PSF, 134s in the spots tables. Then properties of all slices are computed, first 134s separately on each IFU to determine the peak position of the mask for 134s each slice and its angle, subsequently the width and horizontal 134s position. Then, the result of all IFUs is analyzed together to produce 134s a refined horizontal position, applying global shifts to each IFU as 134s needed. The vertical position is then determined using the known slice 134s ordering on the sky; the relative peak positions are put into 134s sequence, taking into account the vertical offsets of the pinholes in 134s the mask. The table is then cleaned up from intermediate debug data. 134s If the --smooth parameter is set to a positive value, it is used to do 134s a sigma-clipped smoothing within each slicer stack, for a more regular 134s appearance of the output table. The table is then saved. As a last 134s optional step, additional raw input data is reduced using the newly 134s geometry to produce an image of the field of view. If these exposures 134s contain smooth features, they can be used as a visual check of the 134s quality of the geometrical calibration. 134s 134s Parameters: 134s ifu1: First IFU to analyze. (int; default: 1) 134s ifu2: Last IFU to analyze. (int; default: 24) 134s sigma: Sigma detection level for spot detection, in terms of 134s median deviation above the median. (float; default: 2.2) 134s centroid: Type of centroiding and FWHM determination to use for all 134s spot measurements: simple barycenter method or using a 134s Gaussian fit. (str; default: 'gaussian') 134s smooth: Use this sigma-level cut for smoothing of the output table 134s within each slicer stack. Set to non-positive value to 134s deactivate smoothing. (float; default: 1.5) 134s lambdamin: When passing any MASK_CHECK frames in the input, use this 134s lower wavelength cut before reconstructing the image. 134s (float; default: 6800.0) 134s lambdamax: When passing any MASK_CHECK frames in the input, use this 134s upper wavelength cut before reconstructing the image. 134s (float; default: 7200.0) 134s 134s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 134s 'TRACE_TABLE', 'WAVECAL_TABLE', 'LINE_CATALOG', 134s 'BADPIX_TABLE', 'MASK_CHECK'] 134s 134s Raw and product frames: 134s MASK --> ['MASK_REDUCED', 'MASK_COMBINED', 'SPOTS_TABLE', 134s 'GEOMETRY_UNSMOOTHED', 'GEOMETRY_TABLE', 'GEOMETRY_CUBE'] 134s Author: Peter Weilbacher 134s 134s 134s Recipe muse_astrometry: 134s version 2.8.7 134s Parameters: {'centroid': 'moffat', 'detsigma': 1.5, 'radius': 3.0, 'faccuracy': 0.0, 'niter': 2, 'rejsigma': 3.0, 'rotcenter': '-0.01,-1.20', 'lambdamin': 4000.0, 'lambdamax': 10000.0, 'lambdaref': 7000.0, 'darcheck': 'none'} 134s Docstring: Compute an astrometric solution. 134s 134s Merge pixel tables from all IFUs, apply correction for differential 134s atmospheric refraction (when necessary), optionally apply flux 134s calibration and telluric correction (if the necessary input data was 134s given), and resample the data from all exposures into a datacube. Use 134s the cube to detect objects which are then matched to their reference 134s positions from which a two-dimensional WCS solution is computed. There 134s are two pattern matching algorithm implemented, which can be selected 134s by chosing a positive or zero value of faccuracy. In the first method 134s (with a positive value of faccuracy), start using the search radius, 134s and iteratively decrease it, until no duplicate detections are 134s identified any more. Similarly, iterate the data accuracy (decrease it 134s downwards from the mean positioning error) until matches are found. 134s Remove the remaining unidentified objects. The second method (when 134s faccuracy is set to zero), iterates through all quadruples in both the 134s detected objects and the catalogue, calculates the transformation and 134s checks whether more than 80% of the detections match a catalog entry 134s within the radius. The main output is the ASTROMETRY_WCS file which is 134s a bare FITS header containing the world coordinate solution. The 134s secondary product is DATACUBE_ASTROMETRY, it is not needed for further 134s processing but can be used for verification and debugging. It contains 134s the reconstructed cube and two images created from it in further FITS 134s extensions: a white-light image and the special image created from the 134s central planes of the cube used to detect and centroid the stars (as 134s well as its variance). 134s 134s Parameters: 134s centroid: Centroiding method to use for objects in the field of 134s view. "gaussian" and "moffat" use 2D fits to derive the 134s centroid, "box" is a simple centroid in a square box. 134s (str; default: 'moffat') 134s detsigma: Source detection sigma level to use. If this is negative, 134s values between its absolute and 1.0 are tested with a 134s stepsize of 0.1, to find an optimal solution. (float; 134s default: 1.5) 134s radius: Initial radius in pixels for pattern matching 134s identification in the astrometric field. (float; default: 134s 3.0) 134s faccuracy: Factor of initial accuracy relative to mean positional 134s accuracy of the measured positions to use for pattern 134s matching. If this is set to zero, use the quadruples based 134s method. (float; default: 0.0) 134s niter: Number of iterations of the astrometric fit. (int; 134s default: 2) 134s rejsigma: Rejection sigma level of the astrometric fit. (float; 134s default: 3.0) 134s rotcenter: Center of rotation of the instrument, given as two comma- 134s separated floating point values in pixels. (str; default: 134s '-0.01,-1.20') 134s lambdamin: Cut off the data below this wavelength after loading the 134s pixel table(s). (float; default: 4000.0) 134s lambdamax: Cut off the data above this wavelength after loading the 134s pixel table(s). (float; default: 10000.0) 134s lambdaref: Reference wavelength used for correction of differential 134s atmospheric refraction. The R-band (peak wavelength ~7000 134s Angstrom) that is usually used for guiding, is close to 134s the central wavelength of MUSE, so a value of 7000.0 134s Angstrom should be used if nothing else is known. A value 134s less than zero switches DAR correction off. (float; 134s default: 7000.0) 134s darcheck: Carry out a check of the theoretical DAR correction using 134s source centroiding. If "correct" it will also apply an 134s empirical correction. (str; default: 'none') 134s 134s Calibration frames: ['ASTROMETRY_REFERENCE', 'EXTINCT_TABLE', 134s 'STD_RESPONSE', 'STD_TELLURIC'] 134s 134s Raw and product frames: 134s PIXTABLE_ASTROMETRY --> ['DATACUBE_ASTROMETRY', 'ASTROMETRY_WCS'] 134s Author: Peter Weilbacher 134s 134s 134s Recipe muse_lingain: 134s version 2.8.7 134s Parameters: {'nifu': 0, 'ybox': 50, 'xgap': 3, 'xborder': 10, 'order': 12, 'toffset': 0.018, 'fluxtol': 0.01, 'sigma': 3.0, 'signalmin': 0.0, 'signalmax': 4.9, 'signalbin': 0.1, 'gainlimit': 100.0, 'gainsigma': 3.0, 'ctsmin': 3.0, 'ctsmax': 4.9, 'ctsbin': 0.1, 'linearmin': 2.5, 'linearmax': 3.0, 'merge': False} 134s Docstring: Compute the gain and a model of the residual non-linearity for each 134s detector quadrant 134s 134s The recipe uses the bias and flat field images of a detector 134s monitoring exposure sequence to determine the detector gain in 134s counts/ADU and to model the residual non-linearity for each of the 134s four detector quadrants of all IFUs. All measurements done by the 134s recipe are done on the illuminated parts of the detector, i.e. on the 134s slices. The location of the slices is taken from the given trace 134s table, which is a mandatory input. Using the traces of the slices on 134s the detector a set of measurement windows is placed along these 134s traces. The data used for the determination of the gain and the 134s residual non-linearity is the taken from these windows. Bad pixels 134s indicated by an, optionally, provided bad pixel table, or flagged 134s during the preprocessing (bias subtraction) of the input data are 134s excluded from the measurements. Local measurements of the read-out- 134s noise, the signal and the gain are calculated for each of the 134s measurement windows. Using these measurements the gain for each 134s detector quadrant is computed as the zero-order coefficient of a 1st 134s order polynomial fitted to the binned gain measurements as a function 134s of the signal level. The residual non-linearity is modelled by a 134s (high) order polynomial which is fitted to the fractional percentage 134s deviation of the count rate from an expected constant count rate (the 134s linear case) as function of the signal level. (Not yet implemented!) 134s 134s Parameters: 134s nifu: IFU to handle. If set to 0, all IFUs are processed 134s serially. If set to -1, all IFUs are processed in 134s parallel. (int; default: 0) 134s ybox: Size of windows along the traces of the slices. (int; 134s default: 50) 134s xgap: Extra offset from tracing edge. (int; default: 3) 134s xborder: Extra offset from the detector edge used for the selection 134s of slices. (int; default: 10) 134s order: Order of the polynomial used to fit the non-linearity 134s residuals. (int; default: 12) 134s toffset: Exposure time offset in seconds to apply to linearity flat 134s fields. (float; default: 0.018) 134s fluxtol: Tolerance value for the overall flux consistency check of 134s a pair of flat fields. The value is the maximum relative 134s offset. (float; default: 0.01) 134s sigma: Sigma value used for signal value clipping. (float; 134s default: 3.0) 134s signalmin: Minimum signal value in log(ADU) used for the gain 134s analysis and the non-linearity polynomial model. (float; 134s default: 0.0) 134s signalmax: Maximum signal value in log(ADU) used for the gain 134s analysis and the non-linearity polynomial model. (float; 134s default: 4.9) 134s signalbin: Size of a signal bin in log10(ADU) used for the gain 134s analysis and the non-linearity polynomial model. (float; 134s default: 0.1) 134s gainlimit: Minimum signal value [ADU] used for fitting the gain 134s relation. (float; default: 100.0) 134s gainsigma: Sigma value for gain value clipping. (float; default: 3.0) 134s ctsmin: Minimum signal value in log(counts) to consider for the 134s non-linearity analysis. (float; default: 3.0) 134s ctsmax: Maximum signal value in log(counts) to consider for the 134s non-linearity analysis. (float; default: 4.9) 134s ctsbin: Size of a signal bin in log10(counts) used for the non- 134s linearity analysis. (float; default: 0.1) 134s linearmin: Lower limit of desired linear range in log10(counts). 134s (float; default: 2.5) 134s linearmax: Upper limit of desired linear range in log10(counts). 134s (float; default: 3.0) 134s merge: Merge output products from different IFUs into a common 134s file. (bool; default: False) 134s 134s Calibration frames: ['MASTER_BIAS', 'TRACE_TABLE', 'BADPIX_TABLE'] 134s 134s Raw and product frames: 134s LINGAIN_LAMP_OFF --> ['NONLINEARITY_GAIN'] 134s LINGAIN_LAMP_ON --> ['NONLINEARITY_GAIN'] 134s Author: Ralf Palsa 134s 134s 134s Recipe muse_qi_mask: 134s version 2.8.7 134s Parameters: {'nifu': 0} 134s Docstring: Create image masks for use with the quick image reconstruction. 134s 134s Trace and wavelength calibration tables (24 of them each, one per IFU) 134s are used to build wavelength maps. If the input data is binned, the 134s wavelength maps are binned in the same way (averaging of pixels). The 134s wavelength maps are then thresholded to create masks of the desired 134s wavelength range. Finally, the mask is "untrimmed", i.e. empty regions 134s for the pre- and overscans are added (in a simple way, assuming 134s quadrants of equal size, and padding of 32 pixels on all quadrant 134s edges). Note: this recipe is not part of the main MUSE pipeline but to 134s be used in the integration phase to create image masks until the 134s system is fully qualified. It therefore does only minimal error 134s checking. 134s 134s Parameters: 134s nifu: IFU to handle. If set to 0, all IFUs are processed serially, 134s which is the recommendation for this recipe, since only then 134s all extensions end up in the same output file. (int; default: 134s 0) 134s 134s Calibration frames: ['TRACE_TABLE', 'WAVECAL_TABLE'] 134s 134s Raw and product frames: 134s BIAS --> ['MASK_IMAGE'] 134s Author: Peter Weilbacher 134s 134s 134s Recipe muse_scipost_combine_pixtables: 134s version 2.8.7 134s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'weight': 'exptime'} 134s Docstring: Combine MUSE pixel tables, either from different IFUs, or from 134s different exposures, or both. 134s 134s Sort pixel tables by exposure and combine them with applied weights 134s into one big pixel table. This is a task separated from muse_scipost. 134s 134s Parameters: 134s lambdamin: Cut off the data below this wavelength after loading the 134s pixel table(s). (float; default: 4000.0) 134s lambdamax: Cut off the data above this wavelength after loading the 134s pixel table(s). (float; default: 10000.0) 134s weight: Type of weighting scheme to use when combining multiple 134s exposures. "exptime" just uses the exposure time to weight 134s the exposures, "fwhm" uses the DIMM information in the 134s header as well, "none" preserves an existing weight column 134s in the input pixel tables without changes. (str; default: 134s 'exptime') 134s 134s Calibration frames: ['OFFSET_LIST'] 134s 134s Raw and product frames: 134s PIXTABLE_OBJECT --> ['PIXTABLE_COMBINED'] 134s Author: Ole Streicher 134s 134s 134s Recipe muse_twilight: 134s version 2.8.7 134s Parameters: {'overscan': 'vpoly', 'ovscreject': 'dcr', 'ovscsigma': 30.0, 'ovscignore': 3, 'combine': 'sigclip', 'nlow': 1, 'nhigh': 1, 'nkeep': 1, 'lsigma': 3.0, 'hsigma': 3.0, 'scale': False, 'resample': 'drizzle', 'crtype': 'median', 'crsigma': 50.0, 'lambdamin': 5000.0, 'lambdamax': 9000.0, 'dlambda': 250.0, 'xorder': 2, 'yorder': 2, 'vignmaskedges': 0.02, 'vignsmooth': 'polyfit', 'vignxpar': -1, 'vignypar': -1, 'vignnfmmask': 22} 134s Docstring: Combine several twilight skyflats into one cube, compute correction 134s factors for each IFU, and create a smooth 3D illumination correction. 134s 134s Processing first handles each raw input image separately: it trims the 134s raw data and records the overscan statistics, subtracts the bias 134s (taking account of the overscan, if --overscan is not "none"), 134s converts the images from adu to count, subtracts the dark, divides by 134s the flat-field and combines all the exposures using input parameters. 134s The input calibrations geometry table, trace table, and wavelength 134s calibration table are used to assign 3D coordinates to each CCD-based 134s pixel, thereby creating a pixel table from the master sky-flat. These 134s pixel tables are then cut in wavelength using the --lambdamin and 134s --lambdamax parameters. The integrated flux in each IFU is computed as 134s the sum of the data in the pixel table, and saved in the header, to be 134s used later as estimate for the relative throughput of each IFU. If an 134s ILLUM exposure was given as input, it is then used to correct the 134s relative illumination between all slices of one IFU. For this, the 134s data of each slice within the pixel table of each IFU is multiplied by 134s the normalized median flux of that slice in the ILLUM exposure. The 134s pixel tables of all IFUs are then merged, using the integrated fluxes 134s as inverse scaling factors, and a cube is reconstructed from the 134s merged dataset, using given parameters. A white-light image is created 134s from the cube. This skyflat cube is then saved to disk, with the 134s white-light image as one extension. To construct a smooth 3D 134s illumination correction, the cube is post-processed in the following 134s way: the white-light image is used to create a mask of the illuminated 134s area. From this area, the optional vignetting mask is removed. The 134s smoothing is then computed for each plane of the cube: the illuminated 134s area is smoothed (by a 5x7 median filter), normalized, fit with a 2D 134s polynomial (of given polynomial orders), and normalized again. A 134s smooth white image is then created by collapsing the smooth cube. If a 134s vignetting mask was given or NFM data is processed, an area close to 134s the edge of the MUSE field is used to compute a 2D correction for the 134s vignetted area: the original unsmoothed white-light image is corrected 134s for large scale gradients by dividing it with the smooth white image. 134s The residuals in the edge area (as defined by the input mask or 134s hardcoded for NFM) are then smoothed using input parameters. This 134s smoothed vignetting correction is the multiplied onto each plane of 134s the smooth cube, normalizing each plane again. This twilight cube is 134s then saved to disk. 134s 134s Parameters: 134s overscan: If this is "none", stop when detecting discrepant 134s overscan levels (see ovscsigma), for "offset" it 134s assumes that the mean overscan level represents the 134s real offset in the bias levels of the exposures 134s involved, and adjusts the data accordingly; for 134s "vpoly", a polynomial is fit to the vertical overscan 134s and subtracted from the whole quadrant. (str; default: 134s 'vpoly') 134s ovscreject: This influences how values are rejected when computing 134s overscan statistics. Either no rejection at all 134s ("none"), rejection using the DCR algorithm ("dcr"), 134s or rejection using an iterative constant fit ("fit"). 134s (str; default: 'dcr') 134s ovscsigma: If the deviation of mean overscan levels between a raw 134s input image and the reference image is higher than 134s |ovscsigma x stdev|, stop the processing. If 134s overscan="vpoly", this is used as sigma rejection 134s level for the iterative polynomial fit (the level 134s comparison is then done afterwards with |100 x stdev| 134s to guard against incompatible settings). Has no effect 134s for overscan="offset". (float; default: 30.0) 134s ovscignore: The number of pixels of the overscan adjacent to the 134s data section of the CCD that are ignored when 134s computing statistics or fits. (int; default: 3) 134s combine: Type of combination to use (str; default: 'sigclip') 134s nlow: Number of minimum pixels to reject with minmax (int; 134s default: 1) 134s nhigh: Number of maximum pixels to reject with minmax (int; 134s default: 1) 134s nkeep: Number of pixels to keep with minmax (int; default: 1) 134s lsigma: Low sigma for pixel rejection with sigclip (float; 134s default: 3.0) 134s hsigma: High sigma for pixel rejection with sigclip (float; 134s default: 3.0) 134s scale: Scale the individual images to a common exposure time 134s before combining them. (bool; default: False) 134s resample: The resampling technique to use for the final output 134s cube. (str; default: 'drizzle') 134s crtype: Type of statistics used for detection of cosmic rays 134s during final resampling. "iraf" uses the variance 134s information, "mean" uses standard (mean/stdev) 134s statistics, "median" uses median and the median median 134s of the absolute median deviation. (str; default: 134s 'median') 134s crsigma: Sigma rejection factor to use for cosmic ray rejection 134s during final resampling. A zero or negative value 134s switches cosmic ray rejection off. (float; default: 134s 50.0) 134s lambdamin: Minimum wavelength for twilight reconstruction. 134s (float; default: 5000.0) 134s lambdamax: Maximum wavelength for twilight reconstruction. 134s (float; default: 9000.0) 134s dlambda: Sampling for twilight reconstruction, this should 134s result in planes of equal wavelength coverage. (float; 134s default: 250.0) 134s xorder: Polynomial order to use in x direction to fit the full 134s field of view. (int; default: 2) 134s yorder: Polynomial order to use in y direction to fit the full 134s field of view. (int; default: 2) 134s vignmaskedges: Pixels on edges stronger than this fraction in the 134s normalized image are excluded from the fit to the 134s vignetted area. Set to non-positive number to include 134s them in the fit. This has no effect for NFM skyflats. 134s (float; default: 0.02) 134s vignsmooth: Type of smoothing to use for the vignetted region 134s given by the VIGNETTING_MASK (for WFM, or the internal 134s mask, for NFM); gaussian uses (vignxpar + vignypar)/2 134s as FWHM. (str; default: 'polyfit') 134s vignxpar: Parameter used by the vignetting smoothing: x order 134s for polyfit (default, recommended 4), parameter that 134s influences the FWHM for the gaussian (recommended: 134s 10), or x dimension of median filter (recommended 5). 134s If a negative value is found, the default is taken. 134s (int; default: -1) 134s vignypar: Parameter used by the vignetting smoothing: y order 134s for polyfit (default, recommended 4), parameter that 134s influences the FWHM for the gaussian (recommended: 134s 10), or y dimension of median filter (recommended 5). 134s If a negative value is found, the default is taken. 134s (int; default: -1) 134s vignnfmmask: The height of the vignetted region at the top of the 134s MUSE field in NFM. This is the region modeled 134s separately (the final vignetting model might be 134s smaller). (int; default: 22) 134s 134s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 134s 'BADPIX_TABLE', 'TRACE_TABLE', 'WAVECAL_TABLE', 134s 'GEOMETRY_TABLE', 'VIGNETTING_MASK'] 134s 134s Raw and product frames: 134s SKYFLAT --> ['DATACUBE_SKYFLAT', 'TWILIGHT_CUBE'] 134s ILLUM --> [] 134s Author: Peter Weilbacher 134s 134s 134s Recipe muse_ampl: 134s version 2.8.7 134s Parameters: {'nifu': 0, 'overscan': 'vpoly', 'ovscreject': 'dcr', 'ovscsigma': 30.0, 'ovscignore': 3, 'combine': 'sigclip', 'nlow': 1, 'nhigh': 1, 'nkeep': 1, 'lsigma': 3.0, 'hsigma': 3.0, 'fbeam': 1.1, 'temp': 3200.0, 'savemaster': False, 'savetable': False, 'merge': False} 134s Docstring: Determine the instrumental throughput from exposures taken with the 134s pico-amplifier / photo diode readings. 134s 134s This recipe combines several separate amplifier images (flat-fields 134s with special FITS headers containing pico amplifier measurements) into 134s one master image file and computes the instrumental throughput per IFU 134s (and slice). Processing trims the raw data and records the overscan 134s statistics, subtracts the bias (taking account of the overscan, if 134s overscan is not "none"), and optionally, the dark from each raw input 134s image, converts them from adu to count, scales them according to their 134s exposure time, and combines them using input parameters. To compute 134s the throughput the image is converted into a pixel table, the flux is 134s then integrated over the given filter band, and the ratio of the 134s expected flux (FITS header INS.AMPL2.CURR) to measured flux is taken, 134s in the same units. If a geometry table was given as input, the 134s relative area of the IFUs is taken into account when computing the 134s flux per unit area. The resulting ratio is the instrument efficiency 134s (throughput) and saved as QC parameters for the whole input image and 134s per slice in the output pixel table. 134s 134s Parameters: 134s nifu: IFU to handle. If set to 0, all IFUs are processed 134s serially. If set to -1, all IFUs are processed in 134s parallel. (int; default: 0) 134s overscan: If this is "none", stop when detecting discrepant 134s overscan levels (see ovscsigma), for "offset" it assumes 134s that the mean overscan level represents the real offset 134s in the bias levels of the exposures involved, and adjusts 134s the data accordingly; for "vpoly", a polynomial is fit to 134s the vertical overscan and subtracted from the whole 134s quadrant. (str; default: 'vpoly') 134s ovscreject: This influences how values are rejected when computing 134s overscan statistics. Either no rejection at all ("none"), 134s rejection using the DCR algorithm ("dcr"), or rejection 134s using an iterative constant fit ("fit"). (str; default: 134s 'dcr') 134s ovscsigma: If the deviation of mean overscan levels between a raw 134s input image and the reference image is higher than 134s |ovscsigma x stdev|, stop the processing. If 134s overscan="vpoly", this is used as sigma rejection level 134s for the iterative polynomial fit (the level comparison is 134s then done afterwards with |100 x stdev| to guard against 134s incompatible settings). Has no effect for 134s overscan="offset". (float; default: 30.0) 134s ovscignore: The number of pixels of the overscan adjacent to the data 134s section of the CCD that are ignored when computing 134s statistics or fits. (int; default: 3) 134s combine: Type of combination to use (str; default: 'sigclip') 134s nlow: Number of minimum pixels to reject with minmax (int; 134s default: 1) 134s nhigh: Number of maximum pixels to reject with minmax (int; 134s default: 1) 134s nkeep: Number of pixels to keep with minmax (int; default: 1) 134s lsigma: Low sigma for pixel rejection with sigclip (float; 134s default: 3.0) 134s hsigma: High sigma for pixel rejection with sigclip (float; 134s default: 3.0) 134s fbeam: Factor to describe the widening of the beam from the 134s focal plane to photo diode 2. (float; default: 1.1) 134s temp: Lamp temperature [K] used to create the black body 134s function. (float; default: 3200.0) 134s savemaster: Save the processed and combined master image before any 134s concolution is done. (bool; default: False) 134s savetable: Save the table with all the processed pixel values. 134s (bool; default: False) 134s merge: Merge output products from different IFUs into a common 134s file. (bool; default: False) 134s 134s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'BADPIX_TABLE', 134s 'GEOMETRY_TABLE', 'FILTER_LIST', 'TRACE_TABLE', 134s 'WAVECAL_TABLE'] 134s 134s Raw and product frames: 134s AMPL --> ['MASTER_AMPL', 'TABLE_AMPL', 'AMPL_CONVOLVED'] 134s Author: Peter Weilbacher 134s 134s 134s Recipe muse_create_sky: 134s version 2.8.7 134s Parameters: {'fraction': 0.75, 'ignore': 0.05, 'sampling': 0.3125, 'csampling': 0.3125, 'crsigma': '15.,15.', 'lambdamin': 4000.0, 'lambdamax': 10000.0, 'lambdaref': 7000.0} 134s Docstring: Create night sky model from selected pixels of an exposure of empty 134s sky. 134s 134s This recipe creates the continuum and the atmospheric transition line 134s spectra of the night sky from the data in a pixel table(s) belonging 134s to one exposure of (mostly) empty sky. 134s 134s Parameters: 134s fraction: Fraction of the image (without the ignored part) to be 134s considered as sky. If an input sky mask is provided, the 134s fraction is applied to the regions within the mask. If the 134s whole sky mask should be used, set this parameter to 1. 134s (float; default: 0.75) 134s ignore: Fraction of the image to be ignored. If an input sky mask 134s is provided, the fraction is applied to the regions within 134s the mask. If the whole sky mask should be used, set this 134s parameter to 0. (float; default: 0.05) 134s sampling: Spectral sampling of the sky spectrum [Angstrom]. (float; 134s default: 0.3125) 134s csampling: Spectral sampling of the continuum spectrum [Angstrom]. 134s (float; default: 0.3125) 134s crsigma: Sigma level clipping for cube-based and spectrum-based CR 134s rejection. This has to be a string of two comma-separated 134s floating-point numbers. The first value gives the sigma- 134s level rejection for cube-based CR rejection (using 134s "median", see muse_scipost), the second value the sigma- 134s level for spectrum-based CR cleaning. Both can be switched 134s off, by passing zero or a negative value. (str; default: 134s '15.,15.') 134s lambdamin: Cut off the data below this wavelength after loading the 134s pixel table(s). (float; default: 4000.0) 134s lambdamax: Cut off the data above this wavelength after loading the 134s pixel table(s). (float; default: 10000.0) 134s lambdaref: Reference wavelength used for correction of differential 134s atmospheric refraction. The R-band (peak wavelength ~7000 134s Angstrom) that is usually used for guiding, is close to 134s the central wavelength of MUSE, so a value of 7000.0 134s Angstrom should be used if nothing else is known. A value 134s less than zero switches DAR correction off. (float; 134s default: 7000.0) 134s 134s Calibration frames: ['EXTINCT_TABLE', 'STD_RESPONSE', 'STD_TELLURIC', 134s 'SKY_LINES', 'SKY_CONTINUUM', 'LSF_PROFILE', 134s 'SKY_MASK'] 134s 134s Raw and product frames: 134s PIXTABLE_SKY --> ['SKY_MASK', 'SKY_IMAGE', 'SKY_SPECTRUM', 134s 'SKY_LINES', 'SKY_CONTINUUM'] 134s Author: Ole Streicher 134s 134s 134s Recipe muse_scipost_subtract_sky: 134s version 2.8.7 134s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'orig': '', 'flux_sky': 0.0, 'flux_lamp': 0.0} 135s Docstring: Subtract night sky model. 135s 135s Subtract the sky as defined by the sky lines and continuum from a 135s pixel table. This is a separated task of muse_scipost. 135s 135s Parameters: 135s lambdamin: Cut off the data below this wavelength after loading the 135s pixel table(s). (float; default: 4000.0) 135s lambdamax: Cut off the data above this wavelength after loading the 135s pixel table(s). (float; default: 10000.0) 135s orig: If specified, write an additional column containing the 135s original data to the pixel table. (str; default: '') 135s flux_sky: Reference flat field flux, obtained by sky exposure. This 135s parameter is needed to scale the data of each pixel table 135s if more than one pixel table was used to determine the 135s sky. By default, it is taken from the parameter ESO DRS 135s MUSE FLAT FLUX SKY of the first pixel table. (float; 135s default: 0.0) 135s flux_lamp: Reference flat field flux, obtained by lamp exposure. This 135s parameter is needed to scale the data of each pixel table 135s if more than one pixel table was used to determine the 135s sky. By default, it is taken from the parameter ESO DRS 135s MUSE FLAT FLUX LAMP of the first pixel table. (float; 135s default: 0.0) 135s 135s Calibration frames: ['SKY_LINES', 'SKY_CONTINUUM', 'LSF_PROFILE'] 135s 135s Raw and product frames: 135s PIXTABLE_REDUCED --> ['PIXTABLE_REDUCED'] 135s Author: Ole Streicher 135s 135s 135s Recipe muse_flat: 135s version 2.8.7 135s Parameters: {'nifu': 0, 'overscan': 'vpoly', 'ovscreject': 'dcr', 'ovscsigma': 30.0, 'ovscignore': 3, 'combine': 'sigclip', 'nlow': 1, 'nhigh': 1, 'nkeep': 1, 'lsigma': 3.0, 'hsigma': 3.0, 'scale': True, 'normalize': True, 'trace': True, 'nsum': 32, 'order': 5, 'edgefrac': 0.5, 'losigmabadpix': 5.0, 'hisigmabadpix': 5.0, 'samples': False, 'merge': False} 135s Docstring: Combine several separate flat images into one master flat file, trace 135s slice locations, and locate dark pixels. 135s 135s This recipe combines several separate flat-field images into one 135s master flat-field file and traces the location of the slices on the 135s CCD. The master flat contains the combined pixel values of the raw 135s flat exposures, with respect to the image combination method used, 135s normalized to the mean flux. The trace table contains polynomials 135s defining the location of the slices on the CCD. Processing trims the 135s raw data and records the overscan statistics, subtracts the bias 135s (taking account of the overscan, if --overscan is not "none"), and 135s optionally, the dark from each raw input image, converts them from adu 135s to count, scales them according to their exposure time, and combines 135s the exposures using input parameters. To trace the position of the 135s slices on the CCD, their edges are located using a threshold method. 135s The edge detection is repeated at given intervals thereby tracing the 135s central position (the mean of both edges) and width of each slit 135s vertically across the CCD. Deviant positions of detections on CCD rows 135s can be detected and excluded before fitting a polynomial to all 135s positions measured for one slice. The polynomial parameters for each 135s slice are saved in the output trace table. Finally, the area between 135s the now known slice edges is searched for dark (and bright) pixels, 135s using statistics in each row of the master flat. 135s 135s Parameters: 135s nifu: IFU to handle. If set to 0, all IFUs are processed 135s serially. If set to -1, all IFUs are processed in 135s parallel. (int; default: 0) 135s overscan: If this is "none", stop when detecting discrepant 135s overscan levels (see ovscsigma), for "offset" it 135s assumes that the mean overscan level represents the 135s real offset in the bias levels of the exposures 135s involved, and adjusts the data accordingly; for 135s "vpoly", a polynomial is fit to the vertical overscan 135s and subtracted from the whole quadrant. (str; default: 135s 'vpoly') 135s ovscreject: This influences how values are rejected when computing 135s overscan statistics. Either no rejection at all 135s ("none"), rejection using the DCR algorithm ("dcr"), 135s or rejection using an iterative constant fit ("fit"). 135s (str; default: 'dcr') 135s ovscsigma: If the deviation of mean overscan levels between a raw 135s input image and the reference image is higher than 135s |ovscsigma x stdev|, stop the processing. If 135s overscan="vpoly", this is used as sigma rejection 135s level for the iterative polynomial fit (the level 135s comparison is then done afterwards with |100 x stdev| 135s to guard against incompatible settings). Has no effect 135s for overscan="offset". (float; default: 30.0) 135s ovscignore: The number of pixels of the overscan adjacent to the 135s data section of the CCD that are ignored when 135s computing statistics or fits. (int; default: 3) 135s combine: Type of combination to use (str; default: 'sigclip') 135s nlow: Number of minimum pixels to reject with minmax (int; 135s default: 1) 135s nhigh: Number of maximum pixels to reject with minmax (int; 135s default: 1) 135s nkeep: Number of pixels to keep with minmax (int; default: 1) 135s lsigma: Low sigma for pixel rejection with sigclip (float; 135s default: 3.0) 135s hsigma: High sigma for pixel rejection with sigclip (float; 135s default: 3.0) 135s scale: Scale the individual images to a common exposure time 135s before combining them. (bool; default: True) 135s normalize: Normalize the master flat to the average flux (bool; 135s default: True) 135s trace: Trace the position of the slices on the master flat 135s (bool; default: True) 135s nsum: Number of lines over which to average when tracing 135s (int; default: 32) 135s order: Order of polynomial fit to the trace (int; default: 5) 135s edgefrac: Fractional change required to identify edge when 135s tracing (float; default: 0.5) 135s losigmabadpix: Low sigma to find dark pixels in the master flat 135s (float; default: 5.0) 135s hisigmabadpix: High sigma to find bright pixels in the master flat 135s (float; default: 5.0) 135s samples: Create a table containing all tracing sample points. 135s (bool; default: False) 135s merge: Merge output products from different IFUs into a 135s common file. (bool; default: False) 135s 135s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'BADPIX_TABLE'] 135s 135s Raw and product frames: 135s FLAT --> ['MASTER_FLAT', 'TRACE_TABLE', 'TRACE_SAMPLES'] 135s Author: Peter Weilbacher (based on Joris Gerssen's draft) 135s 135s 135s Recipe muse_illum: 135s version 2.8.7 135s Parameters: {} 135s Docstring: Dummy recipe to convert a raw illumination flat field into a DFS 135s product 135s 135s The recipe copies the data of an illumination flat-field unmodified to 135s the output file. However it alters the header data such that the 135s result is a DFS compliant product file, which can be used in the on- 135s line pipeline environment to correct the illumination of twilight 135s and/or science observations. This recipe has no use in any environment 135s other than the on-line pipeline environment! 135s 135s No parameters 135s Calibration frames: [] 135s 135s Raw and product frames: 135s ILLUMFLAT --> ['ILLUM'] 135s Author: Ralf Palsa 135s 135s 135s Recipe muse_wavecal: 135s version 2.8.7 135s Parameters: {'nifu': 0, 'overscan': 'vpoly', 'ovscreject': 'dcr', 'ovscsigma': 30.0, 'ovscignore': 3, 'combine': 'sigclip', 'lampwise': True, 'sigma': 1.0, 'dres': 0.05, 'tolerance': 0.1, 'xorder': 2, 'yorder': 6, 'linesigma': -1.0, 'residuals': False, 'fitsigma': -1.0, 'fitweighting': 'cerrscatter', 'saveimages': False, 'resample': False, 'wavemap': False, 'merge': False} 135s Docstring: Detect arc emission lines and determine the wavelength solution for 135s each slice. 135s 135s This recipe detects arc emission lines and fits a wavelength solution 135s to each slice of the instrument. The wavelength calibration table 135s contains polynomials defining the wavelength solution of the slices on 135s the CCD. Processing trims the raw data and records the overscan 135s statistics, subtracts the bias (taking account of the overscan, if 135s --overscan is not "none") and converts them from adu to count. 135s Optionally, the dark can be subtracted and the data can be divided by 135s the flat-field, but this is not recommended. The data is then combined 135s using input parameters, into separate images for each lamp. To compute 135s the wavelength solution, arc lines are detected at the center of each 135s slice (using threshold detection on a S/N image) and subsequently 135s assigned wavelengths, using pattern matching to identify lines from 135s the input line catalog. Each line is then traced to the edges of the 135s slice, using Gaussian centering in each CCD column. The Gaussians not 135s only yield center, but also centering error, and line properties (e.g. 135s FWHM). Deviant fits are detected using polynomial fits to each arc 135s line (using the xorder parameter) and rejected. These analysis and 135s measuring steps are carried out separately on images exposed by the 135s different arc lamps, reducing the amount of blending, that can 135s otherwise influence line identification and Gaussian centering. The 135s final two-dimensional fit uses all positions (of all lamps), their 135s wavelengths, and the given polynomial orders to compute the final 135s wavelength solution for each slice, iteratively rejecting outliers. 135s This final fit can be either unweighted (fitweighting="uniform", for 135s fastest processing) or weighted (other values of fitweighting, for 135s higher accuracy). 135s 135s Parameters: 135s nifu: IFU to handle. If set to 0, all IFUs are processed 135s serially. If set to -1, all IFUs are processed in 135s parallel. (int; default: 0) 135s overscan: If this is "none", stop when detecting discrepant 135s overscan levels (see ovscsigma), for "offset" it 135s assumes that the mean overscan level represents the 135s real offset in the bias levels of the exposures 135s involved, and adjusts the data accordingly; for 135s "vpoly", a polynomial is fit to the vertical overscan 135s and subtracted from the whole quadrant. (str; default: 135s 'vpoly') 135s ovscreject: This influences how values are rejected when computing 135s overscan statistics. Either no rejection at all 135s ("none"), rejection using the DCR algorithm ("dcr"), or 135s rejection using an iterative constant fit ("fit"). 135s (str; default: 'dcr') 135s ovscsigma: If the deviation of mean overscan levels between a raw 135s input image and the reference image is higher than 135s |ovscsigma x stdev|, stop the processing. If 135s overscan="vpoly", this is used as sigma rejection level 135s for the iterative polynomial fit (the level comparison 135s is then done afterwards with |100 x stdev| to guard 135s against incompatible settings). Has no effect for 135s overscan="offset". (float; default: 30.0) 135s ovscignore: The number of pixels of the overscan adjacent to the 135s data section of the CCD that are ignored when computing 135s statistics or fits. (int; default: 3) 135s combine: Type of lampwise image combination to use. (str; 135s default: 'sigclip') 135s lampwise: Identify and measure the arc emission lines on images 135s separately for each lamp setup. (bool; default: True) 135s sigma: Sigma level used to detect arc emission lines above the 135s median background level in the S/N image of the central 135s column of each slice (float; default: 1.0) 135s dres: The allowed range of resolutions for pattern matching 135s (of detected arc lines to line list) in fractions 135s relative to the expected value (float; default: 0.05) 135s tolerance: Tolerance for pattern matching (of detected arc lines 135s to line list) (float; default: 0.1) 135s xorder: Order of the polynomial for the horizontal curvature 135s within each slice (int; default: 2) 135s yorder: Order of the polynomial used to fit the dispersion 135s relation (int; default: 6) 135s linesigma: Sigma level for iterative rejection of deviant fits for 135s each arc line within each slice, a negative value means 135s to use the default (2.5). (float; default: -1.0) 135s residuals: Create a table containing residuals of the fits to the 135s data of all arc lines. This is useful to assess the 135s quality of the wavelength solution in detail. (bool; 135s default: False) 135s fitsigma: Sigma level for iterative rejection of deviant 135s datapoints during the final polynomial wavelength 135s solution within each slice, a negative value means to 135s use the default (3.0). (float; default: -1.0) 135s fitweighting: Type of weighting to use in the final polynomial 135s wavelength solution fit, using centroiding error 135s estimate and/or scatter of each single line as 135s estimates of its accuracy. (str; default: 135s 'cerrscatter') 135s saveimages: Save (bool; default: False) 135s resample: Resample the input arc images onto 2D images for a 135s visual check using tracing and wavelength calibration 135s solutions. Note that the image produced will show small 135s wiggles even when the calibration was successful! 135s (bool; default: False) 135s wavemap: Create a wavelength map of the input images (bool; 135s default: False) 135s merge: Merge output products from different IFUs into a common 135s file. (bool; default: False) 135s 135s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 135s 'TRACE_TABLE', 'LINE_CATALOG', 'BADPIX_TABLE'] 135s 135s Raw and product frames: 135s ARC --> ['WAVECAL_TABLE', 'WAVECAL_RESIDUALS', 'ARC_RED_LAMP'] 135s Author: Peter Weilbacher 135s 135s 135s Recipe muse_scipost_raman: 135s version 2.8.7 135s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'lambdaref': 7000.0, 'width': 20.0, 'crsigma': 15.0, 'fraction': 0.75, 'ignore': 0.05} 135s Docstring: Remove of 4GLSF Raman emission. 135s 135s This recipe removes the Raman scattered light of the 4GLSF system from 135s the exposure. It must be before the normal sky subtraction. 135s 135s Parameters: 135s lambdamin: Cut off the data below this wavelength after loading the 135s pixel table(s). (float; default: 4000.0) 135s lambdamax: Cut off the data above this wavelength after loading the 135s pixel table(s). (float; default: 10000.0) 135s lambdaref: Reference wavelength used for correction of differential 135s atmospheric refraction. The R-band (peak wavelength ~7000 135s Angstrom) that is usually used for guiding, is close to 135s the central wavelength of MUSE, so a value of 7000.0 135s Angstrom should be used if nothing else is known. A value 135s less than zero switches DAR correction off. (float; 135s default: 7000.0) 135s width: Wavelength range around Raman lines [Angstrom]. (float; 135s default: 20.0) 135s crsigma: Sigma level clipping for cube-based CR rejection (using 135s "median", see muse_scipost). It can be switched off, by 135s passing zero or a negative value. (float; default: 15.0) 135s fraction: Fraction of the image (without the ignored part) to be 135s considered as sky. If an input sky mask is provided, the 135s fraction is applied to the regions within the mask. If the 135s whole sky mask should be used, set this parameter to 1. 135s (float; default: 0.75) 135s ignore: Lowest fraction of the image to be ignored. If an input 135s sky mask is provided, the fraction is applied to the 135s regions within the mask. If the whole sky mask should be 135s used, set this parameter to 0. (float; default: 0.05) 135s 135s Calibration frames: ['RAMAN_LINES', 'LSF_PROFILE', 'SKY_MASK'] 135s 135s Raw and product frames: 135s PIXTABLE_OBJECT --> ['RAMAN_IMAGES', 'PIXTABLE_REDUCED'] 135s Author: Ole Streicher 135s 135s 135s Recipe muse_dark: 135s version 2.8.7 135s Parameters: {'nifu': 0, 'overscan': 'vpoly', 'ovscreject': 'dcr', 'ovscsigma': 30.0, 'ovscignore': 3, 'combine': 'sigclip', 'nlow': 1, 'nhigh': 1, 'nkeep': 1, 'lsigma': 3.0, 'hsigma': 3.0, 'scale': True, 'normalize': 3600.0, 'hotsigma': 5.0, 'model': False, 'merge': False} 135s Docstring: Combine several separate dark images into one master dark file and 135s locate hot pixels. 135s 135s This recipe combines several separate dark images into one master dark 135s file. The master dark contains the combined pixel values of the raw 135s dark exposures, with respect to the image combination method used and 135s normalization time specified. Processing trims the raw data and 135s records the overscan statistics, subtracts the bias (taking account of 135s the overscan, if --overscan is not "none") from each raw input image, 135s converts them from adu to count, scales them according to their 135s exposure time, and combines them using input parameters. Hot pixels 135s are then identified using image statistics and marked in the data 135s quality extension. The combined image is normalized to 1 hour exposure 135s time. QC statistics are computed on the output master dark. If 135s --model=true, a smooth polynomial model of the combined master dark is 135s computed, created from several individual 2D polynomials to describe 135s different features visible in MUSE dark frames. It is only advisable 135s to use this, if the master dark is the result of at least 50 135s individual long dark exposures. 135s 135s Parameters: 135s nifu: IFU to handle. If set to 0, all IFUs are processed 135s serially. If set to -1, all IFUs are processed in 135s parallel. (int; default: 0) 135s overscan: If this is "none", stop when detecting discrepant 135s overscan levels (see ovscsigma), for "offset" it assumes 135s that the mean overscan level represents the real offset 135s in the bias levels of the exposures involved, and adjusts 135s the data accordingly; for "vpoly", a polynomial is fit to 135s the vertical overscan and subtracted from the whole 135s quadrant. (str; default: 'vpoly') 135s ovscreject: This influences how values are rejected when computing 135s overscan statistics. Either no rejection at all ("none"), 135s rejection using the DCR algorithm ("dcr"), or rejection 135s using an iterative constant fit ("fit"). (str; default: 135s 'dcr') 135s ovscsigma: If the deviation of mean overscan levels between a raw 135s input image and the reference image is higher than 135s |ovscsigma x stdev|, stop the processing. If 135s overscan="vpoly", this is used as sigma rejection level 135s for the iterative polynomial fit (the level comparison is 135s then done afterwards with |100 x stdev| to guard against 135s incompatible settings). Has no effect for 135s overscan="offset". (float; default: 30.0) 135s ovscignore: The number of pixels of the overscan adjacent to the data 135s section of the CCD that are ignored when computing 135s statistics or fits. (int; default: 3) 135s combine: Type of image combination to use. (str; default: 135s 'sigclip') 135s nlow: Number of minimum pixels to reject with minmax. (int; 135s default: 1) 135s nhigh: Number of maximum pixels to reject with minmax. (int; 135s default: 1) 135s nkeep: Number of pixels to keep with minmax. (int; default: 1) 135s lsigma: Low sigma for pixel rejection with sigclip. (float; 135s default: 3.0) 135s hsigma: High sigma for pixel rejection with sigclip. (float; 135s default: 3.0) 135s scale: Scale the individual images to a common exposure time 135s before combining them. (bool; default: True) 135s normalize: Normalize the master dark to this exposure time (in 135s seconds). To disable normalization, set this to a 135s negative value. (float; default: 3600.0) 135s hotsigma: Sigma level, in terms of median deviation above the 135s median dark level, above which a pixel is detected and 135s marked as 'hot'. (float; default: 5.0) 135s model: Model the master dark using a set of polynomials. (bool; 135s default: False) 135s merge: Merge output products from different IFUs into a common 135s file. (bool; default: False) 135s 135s Calibration frames: ['MASTER_BIAS', 'BADPIX_TABLE'] 135s 135s Raw and product frames: 135s DARK --> ['MASTER_DARK', 'MODEL_DARK'] 135s Author: Peter Weilbacher 135s 135s 135s Recipe muse_scipost_apply_astrometry: 135s version 2.8.7 135s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0} 135s Docstring: Calibrate astrometry for MUSE pixel tables. 135s 135s Apply an astrometric calibration to the pixel table spatial 135s coordinates. This is a task separated from muse_scipost. 135s 135s Parameters: 135s lambdamin: Cut off the data below this wavelength after loading the 135s pixel table(s). (float; default: 4000.0) 135s lambdamax: Cut off the data above this wavelength after loading the 135s pixel table(s). (float; default: 10000.0) 135s 135s Calibration frames: ['ASTROMETRY_WCS'] 135s 135s Raw and product frames: 135s PIXTABLE_OBJECT --> ['PIXTABLE_OBJECT'] 135s Author: Ole Streicher 135s 135s 135s Recipe muse_scipost_calibrate_flux: 135s version 2.8.7 135s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0} 135s Docstring: Calibrate flux for MUSE pixel tables. 135s 135s Replace the intensity in the MUSE pixel tables by the absolute flux. 135s This is a task separated from muse_scipost. 135s 135s Parameters: 135s lambdamin: Cut off the data below this wavelength after loading the 135s pixel table(s). (float; default: 4000.0) 135s lambdamax: Cut off the data above this wavelength after loading the 135s pixel table(s). (float; default: 10000.0) 135s 135s Calibration frames: ['EXTINCT_TABLE', 'STD_RESPONSE', 'STD_TELLURIC'] 135s 135s Raw and product frames: 135s PIXTABLE_OBJECT --> ['PIXTABLE_OBJECT'] 135s Author: Ole Streicher 135s 135s 135s Recipe muse_exp_combine: 135s version 2.8.7 135s Parameters: {'save': 'cube', 'resample': 'drizzle', 'dx': 0.0, 'dy': 0.0, 'dlambda': 0.0, 'crtype': 'median', 'crsigma': 10.0, 'rc': 1.25, 'pixfrac': '0.6,0.6', 'ld': 1, 'format': 'Cube', 'weight': 'exptime', 'filter': 'white', 'lambdamin': 4000.0, 'lambdamax': 10000.0} 135s Docstring: Combine several exposures into one datacube. 135s 135s Sort reduced pixel tables, one per exposure, by exposure and combine 135s them with applied weights into one final datacube. 135s 135s Parameters: 135s save: Select output product(s) to save. Can contain one or more 135s of "cube" (output cube and associated images; if this is 135s not given, no resampling is done at all) or "combined" 135s (fully reduced and combined pixel table for the full set 135s of exposures; this is useful, if the final resampling step 135s is to be done again separately). If several options are 135s given, they have to be comma-separated. (str; default: 135s 'cube') 135s resample: The resampling technique to use for the final output cube. 135s (str; default: 'drizzle') 135s dx: Horizontal step size for resampling (in arcsec or pixel). 135s The following defaults are taken when this value is set to 135s 0.0: 0.2'' for WFM, 0.025'' for NFM, 1.0 if data is in 135s pixel units. (float; default: 0.0) 135s dy: Vertical step size for resampling (in arcsec or pixel). 135s The following defaults are taken when this value is set to 135s 0.0: 0.2'' for WFM, 0.025'' for NFM, 1.0 if data is in 135s pixel units. (float; default: 0.0) 135s dlambda: Wavelength step size (in Angstrom). Natural instrument 135s sampling is used, if this is 0.0 (float; default: 0.0) 135s crtype: Type of statistics used for detection of cosmic rays 135s during final resampling. "iraf" uses the variance 135s information, "mean" uses standard (mean/stdev) statistics, 135s "median" uses median and the median median of the absolute 135s median deviation. (str; default: 'median') 135s crsigma: Sigma rejection factor to use for cosmic ray rejection 135s during final resampling. A zero or negative value switches 135s cosmic ray rejection off. (float; default: 10.0) 135s rc: Critical radius for the "renka" resampling method. (float; 135s default: 1.25) 135s pixfrac: Pixel down-scaling factor for the "drizzle" resampling 135s method. Up to three, comma-separated, floating-point 135s values can be given. If only one value is given, it 135s applies to all dimensions, two values are interpreted as 135s spatial and spectral direction, respectively, while three 135s are taken as horizontal, vertical, and spectral. (str; 135s default: '0.6,0.6') 135s ld: Number of adjacent pixels to take into account during 135s resampling in all three directions (loop distance); this 135s affects all resampling methods except "nearest". (int; 135s default: 1) 135s format: Type of output file format, "Cube" is a standard FITS cube 135s with NAXIS=3 and multiple extensions (for data and 135s variance). The extended "x" formats include the 135s reconstructed image(s) in FITS image extensions within the 135s same file. "sdpCube" does some extra calculations to 135s create FITS keywords for the ESO Science Data Products. 135s (str; default: 'Cube') 135s weight: Type of weighting scheme to use when combining multiple 135s exposures. "exptime" just uses the exposure time to weight 135s the exposures, "fwhm" uses the best available seeing 135s information from the headers as well, "header" queries 135s ESO.DRS.MUSE.WEIGHT of each input file instead of the 135s FWHM, and "none" preserves an existing weight column in 135s the input pixel tables without changes. (str; default: 135s 'exptime') 135s filter: The filter name(s) to be used for the output field-of-view 135s image. Each name has to correspond to an EXTNAME in an 135s extension of the FILTER_LIST file. If an unsupported 135s filter name is given, creation of the respective image is 135s omitted. If multiple filter names are given, they have to 135s be comma separated. (str; default: 'white') 135s lambdamin: Cut off the data below this wavelength after loading the 135s pixel table(s). (float; default: 4000.0) 135s lambdamax: Cut off the data above this wavelength after loading the 135s pixel table(s). (float; default: 10000.0) 135s 135s Calibration frames: ['OFFSET_LIST', 'FILTER_LIST', 'OUTPUT_WCS'] 135s 135s Raw and product frames: 135s PIXTABLE_REDUCED --> ['DATACUBE_FINAL', 'IMAGE_FOV', 135s 'PIXTABLE_COMBINED'] 135s Author: Peter Weilbacher 135s 135s 135s Recipe muse_scipost: 135s version 2.8.7 135s Parameters: {'save': 'cube,skymodel', 'resample': 'drizzle', 'dx': 0.0, 'dy': 0.0, 'dlambda': 0.0, 'crtype': 'median', 'crsigma': 15.0, 'rc': 1.25, 'pixfrac': '0.8,0.8', 'ld': 1, 'format': 'Cube', 'weight': 'exptime', 'filter': 'white', 'autocalib': 'none', 'raman_width': 20.0, 'skymethod': 'model', 'lambdamin': 4000.0, 'lambdamax': 10000.0, 'lambdaref': 7000.0, 'darcheck': 'none', 'skymodel_fraction': 0.1, 'skymodel_ignore': 0.05, 'skymodel_sampling': 0.3125, 'skymodel_csampling': 0.3125, 'sky_crsigma': '15.,15.', 'rvcorr': 'bary', 'astrometry': True} 135s Docstring: Prepare reduced and combined science products. 135s 135s Sort input pixel tables into lists of files per exposure, merge pixel 135s tables from all IFUs of each exposure. Correct each exposure for 135s differential atmospheric refraction (unless --lambdaref is far outside 135s the MUSE wavelength range, or NFM is used which has a built-in 135s corrector). Then the flux calibration is carried out, if a response 135s curve was given in the input; it includes a correction of telluric 135s absorption, if a telluric absorption correction file was given. If 135s observations were done with AO and a RAMAN_LINES file was given, a 135s procedure is run to clean the Raman scattering emission lines from the 135s data. Next, the slice autocalibration is computed and the flux 135s correction factors are applied to the pixel table (if 135s --autocalib="deepfield"). If user-provided autocalibration is 135s requested (--autocalib="user"), then the autocalibration is not 135s computed on the input exposure but the autocalibration factors are 135s read from the AUTOCAL_FACTORS table and applied directly to the data. 135s Then the sky subtraction is carried out (unless --skymethod="none"), 135s either directly subtracting an input sky continuum and an input sky 135s emission lines (for --skymethod="subtract-model"), or 135s (--skymethod="model") create a sky spectrum from the darkest fraction 135s (--skymodel_fraction, after ignoring the lowest --skymodel_ignore as 135s artifacts) of the field of view, then fitting and subtracting sky 135s emission lines using an initial estimate of the input sky lines; then 135s the continuum (residuals after subtracting the sky lines from the sky 135s spectrum) is subtracted as well. If --save contains "skymodel", all 135s sky-related products are saved for each exposure. Afterwards the data 135s is corrected for the radial velocity of the observer (--rvcorr), 135s before the input (or a default) astrometric solution is applied. Now 135s each individual exposure is fully reduced; the pixel tables at this 135s stage can be saved by setting "individual" in --save. If multiple 135s exposures were given, they are then combined. If --save contains 135s "combined", this final merged pixel table is saved. Finally (if --save 135s contains "cube"), the data is resampled into a datacube, using all 135s parameters given to the recipe. The extent and orientation of the cube 135s is normally computed from the data itself, but this can be overridden 135s by passing a file with the output world coordinate system 135s (OUTPUT_WCS), for example a MUSE cube. This can also be used to sample 135s the wavelength axis logarithmically (in that file set "CTYPE3='AWAV- 135s LOG'"). As a last step, the computed cube is integrated over all 135s filter functions given (--filter) that are also present in the input 135s filter list table. 135s 135s Parameters: 135s save: Select output product(s) to save. Can contain one 135s or more of "cube", "autocal", "skymodel", 135s "individual", "positioned", "combined", and 135s "stacked". If several options are given, they 135s have to be comma- separated. ("cube": output cube 135s and associated images, if this is not given, no 135s final resampling is done at all -- "autocal": up 135s to two additional output products related to the 135s slice autocalibration -- "raman": up to four 135s additional output products about the Raman light 135s distribution for AO observations -- "skymodel": 135s up to four additional output products about the 135s effectively used sky that was subtracted with the 135s "model" method -- "individual": fully reduced 135s pixel table for each individual exposure -- 135s "positioned": fully reduced and positioned pixel 135s table for each individual exposure, the 135s difference to "individual" is that here, the 135s output pixel tables have coordinates in RA and 135s DEC, and the optional offsets were applied; this 135s is only useful, if both the relative exposure 135s weighting and the final resampling are to be done 135s externally -- "combined": fully reduced and 135s combined pixel table for the full set of 135s exposures, the difference to "positioned" is that 135s all pixel tables are combined into one, with an 135s added weight column; this is useful, if only the 135s final resampling step is to be done separately -- 135s "stacked": an additional output file in form of a 135s 2D column-stacked image, i.e. x direction is 135s pseudo-spatial, y direction is wavelength.) (str; 135s default: 'cube,skymodel') 135s resample: The resampling technique to use for the final 135s output cube. (str; default: 'drizzle') 135s dx: Horizontal step size for resampling (in arcsec or 135s pixel). The following defaults are taken when 135s this value is set to 0.0: 0.2'' for WFM, 0.025'' 135s for NFM, 1.0 if data is in pixel units. (float; 135s default: 0.0) 135s dy: Vertical step size for resampling (in arcsec or 135s pixel). The following defaults are taken when 135s this value is set to 0.0: 0.2'' for WFM, 0.025'' 135s for NFM, 1.0 if data is in pixel units. (float; 135s default: 0.0) 135s dlambda: Wavelength step size (in Angstrom). Natural 135s instrument sampling is used, if this is 0.0 135s (float; default: 0.0) 135s crtype: Type of statistics used for detection of cosmic 135s rays during final resampling. "iraf" uses the 135s variance information, "mean" uses standard 135s (mean/stdev) statistics, "median" uses median and 135s the median median of the absolute median 135s deviation. (str; default: 'median') 135s crsigma: Sigma rejection factor to use for cosmic ray 135s rejection during final resampling. A zero or 135s negative value switches cosmic ray rejection off. 135s (float; default: 15.0) 135s rc: Critical radius for the "renka" resampling 135s method. (float; default: 1.25) 135s pixfrac: Pixel down-scaling factor for the "drizzle" 135s resampling method. Up to three, comma-separated, 135s floating-point values can be given. If only one 135s value is given, it applies to all dimensions, two 135s values are interpreted as spatial and spectral 135s direction, respectively, while three are taken as 135s horizontal, vertical, and spectral. (str; 135s default: '0.8,0.8') 135s ld: Number of adjacent pixels to take into account 135s during resampling in all three directions (loop 135s distance); this affects all resampling methods 135s except "nearest". (int; default: 1) 135s format: Type of output file format, "Cube" is a standard 135s FITS cube with NAXIS=3 and multiple extensions 135s (for data and variance). The extended "x" formats 135s include the reconstructed image(s) in FITS image 135s extensions within the same file. "sdpCube" does 135s some extra calculations to create FITS keywords 135s for the ESO Science Data Products. (str; default: 135s 'Cube') 135s weight: Type of weighting scheme to use when combining 135s multiple exposures. "exptime" just uses the 135s exposure time to weight the exposures, "fwhm" 135s uses the best available seeing information from 135s the headers as well, "none" preserves an existing 135s weight column in the input pixel tables without 135s changes. (str; default: 'exptime') 135s filter: The filter name(s) to be used for the output 135s field-of-view image. Each name has to correspond 135s to an EXTNAME in an extension of the FILTER_LIST 135s file. If an unsupported filter name is given, 135s creation of the respective image is omitted. If 135s multiple filter names are given, they have to be 135s comma separated. (str; default: 'white') 135s autocalib: The type of autocalibration to use. "none" 135s switches it off, "deepfield" uses the revised 135s MPDAF method that can be used for the reduction 135s of mostly empty "Deep Fields", "user" searches 135s for a user- provided table with autocalibration 135s factors. (str; default: 'none') 135s raman_width: Wavelength range around Raman lines [Angstrom]. 135s (float; default: 20.0) 135s skymethod: The method used to subtract the sky background 135s (spectrum). Option "model" should work in all 135s kinds of science fields: it uses a global sky 135s spectrum model with a local LSF. "model" uses 135s fluxes indicated in the SKY_LINES file as 135s starting estimates, but re-fits them on the 135s global sky spectrum created from the science 135s exposure. If SKY_CONTINUUM is given, it is 135s directly subtracted, otherwise it is created from 135s the sky region of the science exposure. Option 135s "subtract- model" uses the input SKY_LINES and 135s SKY_CONTINUUM, subtracting them directly without 135s re-fitting the fluxes, but still makes use of the 135s local LSF, hence LSF_PROFILE is required. The 135s inputs LSF_PROFILE and SKY_LINES are necessary 135s for these two model-based methods; SKY_CONTINUUM 135s is required for "subtract-model" and optional for 135s "model"; SKY_MASK is optional for "model". 135s Finally, option "simple" creates a sky spectrum 135s from the science data, and directly subtracts it, 135s without taking the LSF into account (LSF_PROFILE 135s and input SKY files are ignored). It works on 135s data that was not flux calibrated. (str; default: 135s 'model') 135s lambdamin: Cut off the data below this wavelength after 135s loading the pixel table(s). (float; default: 135s 4000.0) 135s lambdamax: Cut off the data above this wavelength after 135s loading the pixel table(s). (float; default: 135s 10000.0) 135s lambdaref: Reference wavelength used for correction of 135s differential atmospheric refraction. The R-band 135s (peak wavelength ~7000 Angstrom) that is usually 135s used for guiding, is close to the central 135s wavelength of MUSE, so a value of 7000.0 Angstrom 135s should be used if nothing else is known. A value 135s less than zero switches DAR correction off. 135s (float; default: 7000.0) 135s darcheck: Carry out a check of the theoretical DAR 135s correction using source centroiding. If "correct" 135s it will also apply an empirical correction. (str; 135s default: 'none') 135s skymodel_fraction: Fraction of the image (without the ignored part) 135s to be considered as sky. If an input sky mask is 135s provided, the fraction is applied to the regions 135s within the mask. If the whole sky mask should be 135s used, set this parameter to 1. (float; default: 135s 0.1) 135s skymodel_ignore: Fraction of the image to be ignored. If an input 135s sky mask is provided, the fraction is applied to 135s the regions within the mask. If the whole sky 135s mask should be used, set this parameter to 0. 135s (float; default: 0.05) 135s skymodel_sampling: Spectral sampling of the sky spectrum [Angstrom]. 135s (float; default: 0.3125) 135s skymodel_csampling: Spectral sampling of the continuum spectrum 135s [Angstrom]. (float; default: 0.3125) 135s sky_crsigma: Sigma level clipping for cube-based and spectrum- 135s based CR rejection when creating the sky 135s spectrum. This has to be a string of two comma- 135s separated floating-point numbers. The first value 135s gives the sigma- level rejection for cube-based 135s CR rejection (using "median"), the second value 135s the sigma-level for spectrum-based CR cleaning. 135s Both can be switched off, by passing zero or a 135s negative value. (str; default: '15.,15.') 135s rvcorr: Correct the radial velocity of the telescope with 135s reference to either the barycenter of the Solar 135s System (bary), the center of the Sun (helio), or 135s to the center of the Earth (geo). (str; default: 135s 'bary') 135s astrometry: If false, skip any astrometric calibration, even 135s if one was passed in the input set of files. This 135s causes creation of an output cube with a linear 135s WCS and may result in errors. If you want to use 135s a sensible default, leave this true but do not 135s pass an ASTROMETRY_WCS. (bool; default: True) 135s 135s Calibration frames: ['EXTINCT_TABLE', 'STD_RESPONSE', 'STD_TELLURIC', 135s 'ASTROMETRY_WCS', 'OFFSET_LIST', 'FILTER_LIST', 135s 'OUTPUT_WCS', 'AUTOCAL_FACTORS', 'RAMAN_LINES', 135s 'SKY_LINES', 'SKY_CONTINUUM', 'LSF_PROFILE', 135s 'SKY_MASK'] 135s 135s Raw and product frames: 135s PIXTABLE_OBJECT --> ['DATACUBE_FINAL', 'IMAGE_FOV', 135s 'OBJECT_RESAMPLED', 'PIXTABLE_REDUCED', 135s 'PIXTABLE_POSITIONED', 'PIXTABLE_COMBINED', 135s 'AUTOCAL_MASK', 'AUTOCAL_FACTORS', 135s 'RAMAN_IMAGES', 'SKY_IMAGE', 'SKY_MASK', 135s 'SKY_SPECTRUM', 'SKY_LINES', 'SKY_CONTINUUM'] 135s Author: Peter Weilbacher 135s 135s 135s Recipe muse_lsf: 135s version 2.8.7 135s Parameters: {'nifu': 0, 'overscan': 'vpoly', 'ovscreject': 'dcr', 'ovscsigma': 30.0, 'ovscignore': 3, 'save_subtracted': False, 'line_quality': 3, 'lsf_range': 7.5, 'lsf_size': 150, 'lambda_size': 30, 'lsf_regression_window': 0.7, 'merge': False, 'combine': 'sigclip', 'method': 'interpolate'} 135s Docstring: Compute the LSF 135s 135s Compute the slice and wavelength dependent LSF from a lines spectrum 135s (ARC lamp). 135s 135s Parameters: 135s nifu: IFU to handle. If set to 0, all IFUs are 135s processed serially. If set to -1, all IFUs are 135s processed in parallel. (int; default: 0) 135s overscan: If this is "none", stop when detecting 135s discrepant overscan levels (see ovscsigma), 135s for "offset" it assumes that the mean overscan 135s level represents the real offset in the bias 135s levels of the exposures involved, and adjusts 135s the data accordingly; for "vpoly", a 135s polynomial is fit to the vertical overscan and 135s subtracted from the whole quadrant. (str; 135s default: 'vpoly') 135s ovscreject: This influences how values are rejected when 135s computing overscan statistics. Either no 135s rejection at all ("none"), rejection using the 135s DCR algorithm ("dcr"), or rejection using an 135s iterative constant fit ("fit"). (str; default: 135s 'dcr') 135s ovscsigma: If the deviation of mean overscan levels 135s between a raw input image and the reference 135s image is higher than |ovscsigma x stdev|, stop 135s the processing. If overscan="vpoly", this is 135s used as sigma rejection level for the 135s iterative polynomial fit (the level comparison 135s is then done afterwards with |100 x stdev| to 135s guard against incompatible settings). Has no 135s effect for overscan="offset". (float; default: 135s 30.0) 135s ovscignore: The number of pixels of the overscan adjacent 135s to the data section of the CCD that are 135s ignored when computing statistics or fits. 135s (int; default: 3) 135s save_subtracted: Save the pixel table after the LSF 135s subtraction. (bool; default: False) 135s line_quality: Minimal quality flag in line catalog for 135s selection (int; default: 3) 135s lsf_range: Wavelength window (half size) around each line 135s to estimate LSF (float; default: 7.5) 135s lsf_size: Image size in LSF direction (int; default: 135s 150) 135s lambda_size: Image size in line wavelength direction (int; 135s default: 30) 135s lsf_regression_window: Size of the regression window in LSF direction 135s (float; default: 0.7) 135s merge: Merge output products from different IFUs into 135s a common file. (bool; default: False) 135s combine: Type of lampwise image combination to use. 135s (str; default: 'sigclip') 135s method: LSF generation method. Depending on this 135s value, either an interpolated LSF cube is 135s created, or a table with the parameters of a 135s hermitean gaussian. (str; default: 135s 'interpolate') 135s 135s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 135s 'TRACE_TABLE', 'WAVECAL_TABLE', 'BADPIX_TABLE', 135s 'LINE_CATALOG'] 135s 135s Raw and product frames: 135s ARC --> ['LSF_PROFILE', 'PIXTABLE_SUBTRACTED'] 135s ARC_LSF --> ['LSF_PROFILE', 'PIXTABLE_SUBTRACTED'] 135s Author: Ole Streicher 135s 135s 135s Recipe muse_bias: 135s version 2.8.7 135s Parameters: {'nifu': 0, 'overscan': 'vpoly', 'ovscreject': 'dcr', 'ovscsigma': 30.0, 'ovscignore': 3, 'combine': 'sigclip', 'nlow': 1, 'nhigh': 1, 'nkeep': 1, 'lsigma': 3.0, 'hsigma': 3.0, 'losigmabadpix': 30.0, 'hisigmabadpix': 3.0, 'merge': False} 135s Docstring: Combine several separate bias images into one master bias file. 135s 135s This recipe combines several separate bias images into one master bias 135s file. The master bias contains the combined pixel values, in adu, of 135s the raw bias exposures, with respect to the image combination method 135s used. Processing trims the raw data and records the overscan 135s statistics, corrects the data levels using the overscan (if overscan 135s is not "none") and combines the exposures using input parameters. The 135s read-out noise is computed for each quadrant of the raw input images 135s and stored as QC parameter. The variance extension is filled with an 135s initial value accordingly, before image combination. Further QC 135s statistics are computed on the output master bias. Additionally, bad 135s columns are searched for and marked in the data quality extension. 135s 135s Parameters: 135s nifu: IFU to handle. If set to 0, all IFUs are processed 135s serially. If set to -1, all IFUs are processed in 135s parallel. (int; default: 0) 135s overscan: If this is "none", stop when detecting discrepant 135s overscan levels (see ovscsigma), for "offset" it 135s assumes that the mean overscan level represents the 135s real offset in the bias levels of the exposures 135s involved, and adjusts the data accordingly; for 135s "vpoly", a polynomial is fit to the vertical overscan 135s and subtracted from the whole quadrant. (str; default: 135s 'vpoly') 135s ovscreject: This influences how values are rejected when computing 135s overscan statistics. Either no rejection at all 135s ("none"), rejection using the DCR algorithm ("dcr"), 135s or rejection using an iterative constant fit ("fit"). 135s (str; default: 'dcr') 135s ovscsigma: If the deviation of mean overscan levels between a raw 135s input image and the reference image is higher than 135s |ovscsigma x stdev|, stop the processing. If 135s overscan="vpoly", this is used as sigma rejection 135s level for the iterative polynomial fit (the level 135s comparison is then done afterwards with |100 x stdev| 135s to guard against incompatible settings). Has no effect 135s for overscan="offset". (float; default: 30.0) 135s ovscignore: The number of pixels of the overscan adjacent to the 135s data section of the CCD that are ignored when 135s computing statistics or fits. (int; default: 3) 135s combine: Type of image combination to use. (str; default: 135s 'sigclip') 135s nlow: Number of minimum pixels to reject with minmax. (int; 135s default: 1) 135s nhigh: Number of maximum pixels to reject with minmax. (int; 135s default: 1) 135s nkeep: Number of pixels to keep with minmax. (int; default: 135s 1) 135s lsigma: Low sigma for pixel rejection with sigclip. (float; 135s default: 3.0) 135s hsigma: High sigma for pixel rejection with sigclip. (float; 135s default: 3.0) 135s losigmabadpix: Low sigma to find dark columns in the combined bias 135s (float; default: 30.0) 135s hisigmabadpix: High sigma to find bright columns in the combined bias 135s (float; default: 3.0) 135s merge: Merge output products from different IFUs into a 135s common file. (bool; default: False) 135s 135s Calibration frames: ['BADPIX_TABLE'] 135s 135s Raw and product frames: 135s BIAS --> ['MASTER_BIAS'] 135s Author: Peter Weilbacher 135s 135s 135s Recipe muse_scipost_make_cube: 135s version 2.8.7 135s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'resample': 'drizzle', 'dx': 0.0, 'dy': 0.0, 'dlambda': 0.0, 'crtype': 'median', 'crsigma': 15.0, 'rc': 1.25, 'pixfrac': '0.8,0.8', 'ld': 1, 'format': 'Cube', 'stacked': False, 'filter': 'white'} 135s Docstring: Make a MUSE cube from a MUSE pixel table. 135s 135s This recipe takes a pixel table and resamples it to either a FITS cube 135s or a Euro3D table and optionally to a stacked spectrum. This is a part 135s of the muse_scipost recipe. 135s 135s Parameters: 135s lambdamin: Cut off the data below this wavelength after loading the 135s pixel table(s). (float; default: 4000.0) 135s lambdamax: Cut off the data above this wavelength after loading the 135s pixel table(s). (float; default: 10000.0) 135s resample: The resampling technique to use for the final output cube. 135s (str; default: 'drizzle') 135s dx: Horizontal step size for resampling (in arcsec or pixel). 135s The following defaults are taken when this value is set to 135s 0.0: 0.2'' for WFM, 0.025'' for NFM, 1.0 if data is in 135s pixel units. (float; default: 0.0) 135s dy: Vertical step size for resampling (in arcsec or pixel). 135s The following defaults are taken when this value is set to 135s 0.0: 0.2'' for WFM, 0.025'' for NFM, 1.0 if data is in 135s pixel units. (float; default: 0.0) 135s dlambda: Wavelength step size (in Angstrom). Natural instrument 135s sampling is used, if this is 0.0 (float; default: 0.0) 135s crtype: Type of statistics used for detection of cosmic rays 135s during final resampling. "iraf" uses the variance 135s information, "mean" uses standard (mean/stdev) statistics, 135s "median" uses median and the median median of the absolute 135s median deviation. (str; default: 'median') 135s crsigma: Sigma rejection factor to use for cosmic ray rejection 135s during final resampling. A zero or negative value switches 135s cosmic ray rejection off. (float; default: 15.0) 135s rc: Critical radius for the "renka" resampling method. (float; 135s default: 1.25) 135s pixfrac: Pixel down-scaling factor for the "drizzle" resampling 135s method. Up to three, comma-separated, floating-point 135s values can be given. If only one value is given, it 135s applies to all dimensions, two values are interpreted as 135s spatial and spectral direction, respectively, while three 135s are taken as horizontal, vertical, and spectral. (str; 135s default: '0.8,0.8') 135s ld: Number of adjacent pixels to take into account during 135s resampling in all three directions (loop distance); this 135s affects all resampling methods except "nearest". (int; 135s default: 1) 135s format: Type of output file format, "Cube" is a standard FITS cube 135s with NAXIS=3 and multiple extensions (for data and 135s variance). The extended "x" formats include the 135s reconstructed image(s) in FITS image extensions within the 135s same file. (str; default: 'Cube') 135s stacked: If true, write an additional output file in form of a 2D 135s stacked image (x direction is pseudo-spatial, y direction 135s is wavelength). (bool; default: False) 135s filter: The filter name(s) to be used for the output field-of-view 135s image. Each name has to correspond to an EXTNAME in an 135s extension of the FILTER_LIST file. If an unsupported 135s filter name is given, creation of the respective image is 135s omitted. If multiple filter names are given, they have to 135s be comma separated. (str; default: 'white') 135s 135s Calibration frames: ['FILTER_LIST', 'OUTPUT_WCS'] 135s 135s Raw and product frames: 135s PIXTABLE_OBJECT --> ['DATACUBE_FINAL', 'IMAGE_FOV', 135s 'OBJECT_RESAMPLED'] 135s Author: Ole Streicher 135s 135s 135s autopkgtest [00:37:05]: test test-recipe.py: -----------------------] 135s autopkgtest [00:37:05]: test test-recipe.py: - - - - - - - - - - results - - - - - - - - - - 135s test-recipe.py PASS (superficial) 135s autopkgtest [00:37:05]: @@@@@@@@@@@@@@@@@@@@ summary 135s test-recipe.py PASS (superficial) 152s Creating nova instance adt-noble-amd64-cpl-plugin-muse-20240326-003449-juju-7f2275-prod-proposed-migration-environment-2 from image adt/ubuntu-noble-amd64-server-20240325.img (UUID ba43860b-557a-4db2-b3f0-378a99bca08c)...