0s autopkgtest [00:53:00]: starting date and time: 2024-04-19 00:53:00+0000 0s autopkgtest [00:53:00]: git checkout: 43bc6cdf gitlab-ci: do not include the salsa pipeline 0s autopkgtest [00:53:00]: host juju-7f2275-prod-proposed-migration-environment-3; command line: /home/ubuntu/autopkgtest/runner/autopkgtest --output-dir /tmp/autopkgtest-work.mmw0jpq0/out --timeout-copy=6000 --setup-commands /home/ubuntu/autopkgtest-cloud/worker-config-production/setup-canonical.sh --apt-pocket=proposed=src:gsl --apt-upgrade cpl-plugin-muse --timeout-short=300 --timeout-copy=20000 --timeout-build=20000 --env=ADT_TEST_TRIGGERS=gsl/2.7.1+dfsg-6ubuntu2 -- ssh -s /home/ubuntu/autopkgtest/ssh-setup/nova -- --flavor autopkgtest --security-groups autopkgtest-juju-7f2275-prod-proposed-migration-environment-3@bos02-arm64-9.secgroup --name adt-noble-arm64-cpl-plugin-muse-20240419-005300-juju-7f2275-prod-proposed-migration-environment-3-281f50e2-1df8-4754-8bde-6ae765045a5d --image adt/ubuntu-noble-arm64-server --keyname testbed-juju-7f2275-prod-proposed-migration-environment-3 --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/ 165s autopkgtest [00:55:45]: testbed dpkg architecture: arm64 166s autopkgtest [00:55:46]: testbed apt version: 2.7.14build2 166s autopkgtest [00:55:46]: @@@@@@@@@@@@@@@@@@@@ test bed setup 167s Get:1 http://ftpmaster.internal/ubuntu noble-proposed InRelease [117 kB] 168s Get:2 http://ftpmaster.internal/ubuntu noble-proposed/main Sources [54.2 kB] 168s Get:3 http://ftpmaster.internal/ubuntu noble-proposed/multiverse Sources [2340 B] 168s Get:4 http://ftpmaster.internal/ubuntu noble-proposed/universe Sources [376 kB] 169s Get:5 http://ftpmaster.internal/ubuntu noble-proposed/restricted Sources [12.2 kB] 169s Get:6 http://ftpmaster.internal/ubuntu noble-proposed/main arm64 Packages [130 kB] 169s Get:7 http://ftpmaster.internal/ubuntu noble-proposed/main arm64 c-n-f Metadata [3144 B] 169s Get:8 http://ftpmaster.internal/ubuntu noble-proposed/restricted arm64 Packages [92.9 kB] 169s Get:9 http://ftpmaster.internal/ubuntu noble-proposed/restricted arm64 c-n-f Metadata [116 B] 169s Get:10 http://ftpmaster.internal/ubuntu noble-proposed/universe arm64 Packages [563 kB] 169s Get:11 http://ftpmaster.internal/ubuntu noble-proposed/universe arm64 c-n-f Metadata [8528 B] 169s Get:12 http://ftpmaster.internal/ubuntu noble-proposed/multiverse arm64 c-n-f Metadata [116 B] 176s Fetched 1360 kB in 2s (561 kB/s) 176s Reading package lists... 178s sh: 4: dhclient: not found 181s Reading package lists... 182s Building dependency tree... 182s Reading state information... 183s Calculating upgrade... 184s The following packages will be upgraded: 184s apport apport-core-dump-handler libkeyutils1 libnuma1 libunwind8 make man-db 184s netcat-openbsd numactl python3-apport python3-problem-report 184s 11 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 184s Need to get 1797 kB of archives. 184s After this operation, 1024 B of additional disk space will be used. 184s Get:1 http://ftpmaster.internal/ubuntu noble/main arm64 python3-problem-report all 2.28.1-0ubuntu1 [23.8 kB] 185s Get:2 http://ftpmaster.internal/ubuntu noble/main arm64 python3-apport all 2.28.1-0ubuntu1 [92.1 kB] 185s Get:3 http://ftpmaster.internal/ubuntu noble/main arm64 apport-core-dump-handler all 2.28.1-0ubuntu1 [16.8 kB] 185s Get:4 http://ftpmaster.internal/ubuntu noble/main arm64 apport all 2.28.1-0ubuntu1 [83.5 kB] 185s Get:5 http://ftpmaster.internal/ubuntu noble/main arm64 libkeyutils1 arm64 1.6.3-3build1 [9654 B] 185s Get:6 http://ftpmaster.internal/ubuntu noble/main arm64 netcat-openbsd arm64 1.226-1ubuntu2 [43.8 kB] 185s Get:7 http://ftpmaster.internal/ubuntu noble/main arm64 libnuma1 arm64 2.0.18-1build1 [23.6 kB] 185s Get:8 http://ftpmaster.internal/ubuntu noble/main arm64 man-db arm64 2.12.0-4build2 [1232 kB] 185s Get:9 http://ftpmaster.internal/ubuntu noble/main arm64 libunwind8 arm64 1.6.2-3build1 [53.5 kB] 185s Get:10 http://ftpmaster.internal/ubuntu noble/main arm64 make arm64 4.3-4.1build2 [178 kB] 185s Get:11 http://ftpmaster.internal/ubuntu noble/main arm64 numactl arm64 2.0.18-1build1 [39.5 kB] 186s Preconfiguring packages ... 186s Fetched 1797 kB in 1s (2350 kB/s) 187s (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 ... 77740 files and directories currently installed.) 187s Preparing to unpack .../00-python3-problem-report_2.28.1-0ubuntu1_all.deb ... 187s Unpacking python3-problem-report (2.28.1-0ubuntu1) over (2.28.0-0ubuntu1) ... 187s Preparing to unpack .../01-python3-apport_2.28.1-0ubuntu1_all.deb ... 187s Unpacking python3-apport (2.28.1-0ubuntu1) over (2.28.0-0ubuntu1) ... 187s Preparing to unpack .../02-apport-core-dump-handler_2.28.1-0ubuntu1_all.deb ... 187s Unpacking apport-core-dump-handler (2.28.1-0ubuntu1) over (2.28.0-0ubuntu1) ... 188s Preparing to unpack .../03-apport_2.28.1-0ubuntu1_all.deb ... 188s Unpacking apport (2.28.1-0ubuntu1) over (2.28.0-0ubuntu1) ... 188s Preparing to unpack .../04-libkeyutils1_1.6.3-3build1_arm64.deb ... 188s Unpacking libkeyutils1:arm64 (1.6.3-3build1) over (1.6.3-3) ... 188s Preparing to unpack .../05-netcat-openbsd_1.226-1ubuntu2_arm64.deb ... 188s Unpacking netcat-openbsd (1.226-1ubuntu2) over (1.226-1ubuntu1) ... 188s Preparing to unpack .../06-libnuma1_2.0.18-1build1_arm64.deb ... 188s Unpacking libnuma1:arm64 (2.0.18-1build1) over (2.0.18-1) ... 188s Preparing to unpack .../07-man-db_2.12.0-4build2_arm64.deb ... 188s Unpacking man-db (2.12.0-4build2) over (2.12.0-4build1) ... 189s Preparing to unpack .../08-libunwind8_1.6.2-3build1_arm64.deb ... 189s Unpacking libunwind8:arm64 (1.6.2-3build1) over (1.6.2-3) ... 189s Preparing to unpack .../09-make_4.3-4.1build2_arm64.deb ... 189s Unpacking make (4.3-4.1build2) over (4.3-4.1build1) ... 189s Preparing to unpack .../10-numactl_2.0.18-1build1_arm64.deb ... 189s Unpacking numactl (2.0.18-1build1) over (2.0.18-1) ... 189s Setting up libkeyutils1:arm64 (1.6.3-3build1) ... 189s Setting up python3-problem-report (2.28.1-0ubuntu1) ... 190s Setting up netcat-openbsd (1.226-1ubuntu2) ... 190s Setting up man-db (2.12.0-4build2) ... 190s Updating database of manual pages ... 196s man-db.service is a disabled or a static unit not running, not starting it. 196s Setting up libunwind8:arm64 (1.6.2-3build1) ... 196s Setting up python3-apport (2.28.1-0ubuntu1) ... 197s Setting up make (4.3-4.1build2) ... 197s Setting up libnuma1:arm64 (2.0.18-1build1) ... 197s Setting up numactl (2.0.18-1build1) ... 197s Setting up apport-core-dump-handler (2.28.1-0ubuntu1) ... 204s Setting up apport (2.28.1-0ubuntu1) ... 204s Installing new version of config file /etc/apport/crashdb.conf ... 207s apport-autoreport.service is a disabled or a static unit not running, not starting it. 208s Processing triggers for libc-bin (2.39-0ubuntu8) ... 209s Reading package lists... 209s Building dependency tree... 209s Reading state information... 211s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 212s Hit:1 http://ftpmaster.internal/ubuntu noble-proposed InRelease 212s Hit:2 http://ftpmaster.internal/ubuntu noble InRelease 212s Hit:3 http://ftpmaster.internal/ubuntu noble-updates InRelease 212s Hit:4 http://ftpmaster.internal/ubuntu noble-security InRelease 217s Reading package lists... 217s Reading package lists... 218s Building dependency tree... 218s Reading state information... 219s Calculating upgrade... 220s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 220s Reading package lists... 221s Building dependency tree... 221s Reading state information... 223s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 223s autopkgtest [00:56:43]: rebooting testbed after setup commands that affected boot 388s autopkgtest-virt-ssh: WARNING: ssh connection failed. Retrying in 3 seconds... 396s autopkgtest [00:59:36]: testbed running kernel: Linux 6.8.0-22-generic #22-Ubuntu SMP PREEMPT_DYNAMIC Fri Apr 5 02:52:09 UTC 2024 400s autopkgtest [00:59:40]: @@@@@@@@@@@@@@@@@@@@ apt-source cpl-plugin-muse 406s Get:1 http://ftpmaster.internal/ubuntu noble/universe cpl-plugin-muse 2.8.7+dfsg-3 (dsc) [2420 B] 406s Get:2 http://ftpmaster.internal/ubuntu noble/universe cpl-plugin-muse 2.8.7+dfsg-3 (tar) [1586 kB] 406s Get:3 http://ftpmaster.internal/ubuntu noble/universe cpl-plugin-muse 2.8.7+dfsg-3 (diff) [14.6 kB] 407s gpgv: Signature made Tue Aug 16 06:12:08 2022 UTC 407s gpgv: using RSA key BAFC6C85F7CB143FEEB6FB157115AFD07710DCF7 407s gpgv: Can't check signature: No public key 407s dpkg-source: warning: cannot verify inline signature for ./cpl-plugin-muse_2.8.7+dfsg-3.dsc: no acceptable signature found 408s autopkgtest [00:59:48]: testing package cpl-plugin-muse version 2.8.7+dfsg-3 408s autopkgtest [00:59:48]: build not needed 432s autopkgtest [01:00:12]: test test-recipe.py: preparing testbed 434s Reading package lists... 434s Building dependency tree... 434s Reading state information... 435s Starting pkgProblemResolver with broken count: 0 435s Starting 2 pkgProblemResolver with broken count: 0 435s Done 437s The following additional packages will be installed: 437s cpl-plugin-muse libblas3 libcext0 libcfitsio10t64 libcplcore26 libcpldfs26 437s libcpldrs26 libcplui26 liberfa1 libfftw3-double3 libfftw3-single3 437s libgfortran5 libgomp1 libgsl27 libgslcblas0 libjs-jquery 437s libjs-jquery-hotkeys libjs-jquery-isonscreen libjs-jquery-metadata 437s libjs-jquery-tablesorter libjs-jquery-throttle-debounce libjs-sphinxdoc 437s libjs-underscore liblapack3 libwcs8 python3-astropy 437s python3-astropy-iers-data python3-coverage python3-cpl python3-dateutil 437s python3-erfa python3-hypothesis python3-iniconfig python3-numpy 437s python3-packaging python3-pluggy python3-ply python3-pytest 437s python3-pytest-arraydiff python3-pytest-astropy 437s python3-pytest-astropy-header python3-pytest-cov python3-pytest-doctestplus 437s python3-pytest-filter-subpackage python3-pytest-mock 437s python3-pytest-remotedata python3-sortedcontainers 437s Suggested packages: 437s cpl-plugin-muse-calib cpl-plugin-muse-doc libfftw3-bin libfftw3-dev 437s gsl-ref-psdoc | gsl-doc-pdf | gsl-doc-info | gsl-ref-html libxml2-utils 437s python-astropy-doc python3-astropy-affiliated python3-bs4 python3-h5py 437s python3-matplotlib python3-pandas python-coverage-doc gdb 437s python-hypothesis-doc gcc gfortran python3-dev python-ply-doc 437s python-pytest-mock-doc python-sortedcontainers-doc 437s Recommended packages: 437s javascript-common libjs-jquery-datatables python3-scipy python3-click 437s The following NEW packages will be installed: 437s autopkgtest-satdep cpl-plugin-muse libblas3 libcext0 libcfitsio10t64 437s libcplcore26 libcpldfs26 libcpldrs26 libcplui26 liberfa1 libfftw3-double3 437s libfftw3-single3 libgfortran5 libgomp1 libgsl27 libgslcblas0 libjs-jquery 437s libjs-jquery-hotkeys libjs-jquery-isonscreen libjs-jquery-metadata 437s libjs-jquery-tablesorter libjs-jquery-throttle-debounce libjs-sphinxdoc 437s libjs-underscore liblapack3 libwcs8 python3-astropy 437s python3-astropy-iers-data python3-coverage python3-cpl python3-dateutil 437s python3-erfa python3-hypothesis python3-iniconfig python3-numpy 437s python3-packaging python3-pluggy python3-ply python3-pytest 437s python3-pytest-arraydiff python3-pytest-astropy 437s python3-pytest-astropy-header python3-pytest-cov python3-pytest-doctestplus 437s python3-pytest-filter-subpackage python3-pytest-mock 437s python3-pytest-remotedata python3-sortedcontainers 437s 0 upgraded, 48 newly installed, 0 to remove and 0 not upgraded. 437s Need to get 18.6 MB/18.6 MB of archives. 437s After this operation, 83.9 MB of additional disk space will be used. 437s Get:1 /tmp/autopkgtest.eO1Ou6/1-autopkgtest-satdep.deb autopkgtest-satdep arm64 0 [724 B] 437s Get:2 http://ftpmaster.internal/ubuntu noble/main arm64 libjs-jquery all 3.6.1+dfsg+~3.5.14-1 [328 kB] 438s Get:3 http://ftpmaster.internal/ubuntu noble/universe arm64 libjs-jquery-hotkeys all 0~20130707+git2d51e3a9+dfsg-2ubuntu2 [11.5 kB] 438s Get:4 http://ftpmaster.internal/ubuntu noble/universe arm64 libcext0 arm64 7.3.2+ds-1build3 [31.6 kB] 438s Get:5 http://ftpmaster.internal/ubuntu noble/universe arm64 libcfitsio10t64 arm64 4.3.1-1.1build2 [520 kB] 438s Get:6 http://ftpmaster.internal/ubuntu noble/main arm64 libgomp1 arm64 14-20240412-0ubuntu1 [144 kB] 439s Get:7 http://ftpmaster.internal/ubuntu noble/main arm64 libfftw3-double3 arm64 3.3.10-1ubuntu3 [384 kB] 439s Get:8 http://ftpmaster.internal/ubuntu noble/main arm64 libfftw3-single3 arm64 3.3.10-1ubuntu3 [583 kB] 439s Get:9 http://ftpmaster.internal/ubuntu noble/universe arm64 libcplcore26 arm64 7.3.2+ds-1build3 [446 kB] 439s Get:10 http://ftpmaster.internal/ubuntu noble/universe arm64 libcplui26 arm64 7.3.2+ds-1build3 [36.5 kB] 439s Get:11 http://ftpmaster.internal/ubuntu noble/universe arm64 libcpldfs26 arm64 7.3.2+ds-1build3 [39.0 kB] 439s Get:12 http://ftpmaster.internal/ubuntu noble/universe arm64 libwcs8 arm64 8.2.2+ds-3build2 [253 kB] 439s Get:13 http://ftpmaster.internal/ubuntu noble/universe arm64 libcpldrs26 arm64 7.3.2+ds-1build3 [62.8 kB] 439s Get:14 http://ftpmaster.internal/ubuntu noble-proposed/universe arm64 libgslcblas0 arm64 2.7.1+dfsg-6ubuntu2 [72.8 kB] 439s Get:15 http://ftpmaster.internal/ubuntu noble-proposed/universe arm64 libgsl27 arm64 2.7.1+dfsg-6ubuntu2 [918 kB] 440s Get:16 http://ftpmaster.internal/ubuntu noble/universe arm64 cpl-plugin-muse arm64 2.8.7+dfsg-3 [523 kB] 440s Get:17 http://ftpmaster.internal/ubuntu noble/main arm64 libblas3 arm64 3.12.0-3build1 [143 kB] 440s Get:18 http://ftpmaster.internal/ubuntu noble/main arm64 libgfortran5 arm64 14-20240412-0ubuntu1 [444 kB] 440s Get:19 http://ftpmaster.internal/ubuntu noble/universe arm64 libjs-jquery-metadata all 12-4 [6582 B] 440s Get:20 http://ftpmaster.internal/ubuntu noble/universe arm64 libjs-jquery-tablesorter all 1:2.31.3+dfsg1-3 [193 kB] 440s Get:21 http://ftpmaster.internal/ubuntu noble/universe arm64 libjs-jquery-throttle-debounce all 1.1+dfsg.1-2 [12.5 kB] 440s Get:22 http://ftpmaster.internal/ubuntu noble/main arm64 libjs-underscore all 1.13.4~dfsg+~1.11.4-3 [118 kB] 440s Get:23 http://ftpmaster.internal/ubuntu noble/main arm64 libjs-sphinxdoc all 7.2.6-6 [149 kB] 440s Get:24 http://ftpmaster.internal/ubuntu noble/main arm64 liblapack3 arm64 3.12.0-3build1 [2241 kB] 441s Get:25 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-iniconfig all 1.1.1-2 [6024 B] 441s Get:26 http://ftpmaster.internal/ubuntu noble/main arm64 python3-packaging all 24.0-1 [41.1 kB] 441s Get:27 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pluggy all 1.4.0-1 [20.4 kB] 441s Get:28 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pytest all 7.4.4-1 [305 kB] 441s Get:29 http://ftpmaster.internal/ubuntu noble/main arm64 python3-dateutil all 2.8.2-3ubuntu1 [79.4 kB] 441s Get:30 http://ftpmaster.internal/ubuntu noble/main arm64 python3-sortedcontainers all 2.4.0-2 [27.6 kB] 441s Get:31 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-hypothesis all 6.98.15-1 [311 kB] 441s Get:32 http://ftpmaster.internal/ubuntu noble/main arm64 python3-numpy arm64 1:1.26.4+ds-6ubuntu1 [3565 kB] 441s Get:33 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pytest-arraydiff all 0.6.1-2 [10.2 kB] 441s Get:34 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pytest-astropy-header all 0.2.2-1 [8190 B] 441s Get:35 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-coverage arm64 7.4.4+dfsg1-0ubuntu2 [148 kB] 441s Get:36 http://ftpmaster.internal/ubuntu noble/universe arm64 libjs-jquery-isonscreen all 1.2.0-1.1 [3244 B] 441s Get:37 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pytest-cov all 4.1.0-1 [21.5 kB] 441s Get:38 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pytest-doctestplus all 1.2.0-1 [23.1 kB] 441s Get:39 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pytest-filter-subpackage all 0.2.0-1 [6094 B] 441s Get:40 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pytest-mock all 3.12.0-1.1 [11.3 kB] 441s Get:41 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pytest-remotedata all 0.4.1-1 [8650 B] 441s Get:42 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pytest-astropy all 0.11.0-1 [5902 B] 441s Get:43 http://ftpmaster.internal/ubuntu noble/main arm64 python3-ply all 3.11-6 [46.5 kB] 441s Get:44 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-astropy-iers-data all 0.2024.01.01.00.33.39-1 [2046 kB] 442s Get:45 http://ftpmaster.internal/ubuntu noble/universe arm64 liberfa1 arm64 2.0.1-1 [136 kB] 442s Get:46 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-erfa arm64 2.0.1.1+ds-3 [311 kB] 442s Get:47 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-astropy arm64 6.0.0-1ubuntu2 [3797 kB] 442s Get:48 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-cpl arm64 0.7.4-2build10 [34.8 kB] 444s Fetched 18.6 MB in 5s (3768 kB/s) 444s Selecting previously unselected package libjs-jquery. 444s (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 ... 77739 files and directories currently installed.) 444s Preparing to unpack .../00-libjs-jquery_3.6.1+dfsg+~3.5.14-1_all.deb ... 444s Unpacking libjs-jquery (3.6.1+dfsg+~3.5.14-1) ... 444s Selecting previously unselected package libjs-jquery-hotkeys. 444s Preparing to unpack .../01-libjs-jquery-hotkeys_0~20130707+git2d51e3a9+dfsg-2ubuntu2_all.deb ... 444s Unpacking libjs-jquery-hotkeys (0~20130707+git2d51e3a9+dfsg-2ubuntu2) ... 444s Selecting previously unselected package libcext0:arm64. 444s Preparing to unpack .../02-libcext0_7.3.2+ds-1build3_arm64.deb ... 444s Unpacking libcext0:arm64 (7.3.2+ds-1build3) ... 444s Selecting previously unselected package libcfitsio10t64:arm64. 444s Preparing to unpack .../03-libcfitsio10t64_4.3.1-1.1build2_arm64.deb ... 444s Unpacking libcfitsio10t64:arm64 (4.3.1-1.1build2) ... 444s Selecting previously unselected package libgomp1:arm64. 444s Preparing to unpack .../04-libgomp1_14-20240412-0ubuntu1_arm64.deb ... 444s Unpacking libgomp1:arm64 (14-20240412-0ubuntu1) ... 445s Selecting previously unselected package libfftw3-double3:arm64. 445s Preparing to unpack .../05-libfftw3-double3_3.3.10-1ubuntu3_arm64.deb ... 445s Unpacking libfftw3-double3:arm64 (3.3.10-1ubuntu3) ... 445s Selecting previously unselected package libfftw3-single3:arm64. 445s Preparing to unpack .../06-libfftw3-single3_3.3.10-1ubuntu3_arm64.deb ... 445s Unpacking libfftw3-single3:arm64 (3.3.10-1ubuntu3) ... 445s Selecting previously unselected package libcplcore26:arm64. 445s Preparing to unpack .../07-libcplcore26_7.3.2+ds-1build3_arm64.deb ... 445s Unpacking libcplcore26:arm64 (7.3.2+ds-1build3) ... 445s Selecting previously unselected package libcplui26:arm64. 445s Preparing to unpack .../08-libcplui26_7.3.2+ds-1build3_arm64.deb ... 445s Unpacking libcplui26:arm64 (7.3.2+ds-1build3) ... 445s Selecting previously unselected package libcpldfs26:arm64. 445s Preparing to unpack .../09-libcpldfs26_7.3.2+ds-1build3_arm64.deb ... 445s Unpacking libcpldfs26:arm64 (7.3.2+ds-1build3) ... 445s Selecting previously unselected package libwcs8:arm64. 445s Preparing to unpack .../10-libwcs8_8.2.2+ds-3build2_arm64.deb ... 445s Unpacking libwcs8:arm64 (8.2.2+ds-3build2) ... 445s Selecting previously unselected package libcpldrs26:arm64. 445s Preparing to unpack .../11-libcpldrs26_7.3.2+ds-1build3_arm64.deb ... 445s Unpacking libcpldrs26:arm64 (7.3.2+ds-1build3) ... 445s Selecting previously unselected package libgslcblas0:arm64. 445s Preparing to unpack .../12-libgslcblas0_2.7.1+dfsg-6ubuntu2_arm64.deb ... 445s Unpacking libgslcblas0:arm64 (2.7.1+dfsg-6ubuntu2) ... 445s Selecting previously unselected package libgsl27:arm64. 446s Preparing to unpack .../13-libgsl27_2.7.1+dfsg-6ubuntu2_arm64.deb ... 446s Unpacking libgsl27:arm64 (2.7.1+dfsg-6ubuntu2) ... 446s Selecting previously unselected package cpl-plugin-muse:arm64. 446s Preparing to unpack .../14-cpl-plugin-muse_2.8.7+dfsg-3_arm64.deb ... 446s Unpacking cpl-plugin-muse:arm64 (2.8.7+dfsg-3) ... 446s Selecting previously unselected package libblas3:arm64. 446s Preparing to unpack .../15-libblas3_3.12.0-3build1_arm64.deb ... 446s Unpacking libblas3:arm64 (3.12.0-3build1) ... 446s Selecting previously unselected package libgfortran5:arm64. 446s Preparing to unpack .../16-libgfortran5_14-20240412-0ubuntu1_arm64.deb ... 446s Unpacking libgfortran5:arm64 (14-20240412-0ubuntu1) ... 446s Selecting previously unselected package 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(0.7.4-2build10) ... 486s Setting up autopkgtest-satdep (0) ... 486s Processing triggers for man-db (2.12.0-4build2) ... 487s Processing triggers for libc-bin (2.39-0ubuntu8) ... 498s (Reading database ... 81627 files and directories currently installed.) 498s Removing autopkgtest-satdep (0) ... 499s autopkgtest [01:01:19]: test test-recipe.py: [----------------------- 501s Recipe muse_lingain: 501s version 2.8.7 501s 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} 501s Docstring: Compute the gain and a model of the residual non-linearity for each 501s detector quadrant 501s 501s The recipe uses the bias and flat field images of a detector 501s monitoring exposure sequence to determine the detector gain in 501s counts/ADU and to model the residual non-linearity for each of the 501s four detector quadrants of all IFUs. All measurements done by the 501s recipe are done on the illuminated parts of the detector, i.e. on the 501s slices. The location of the slices is taken from the given trace 501s table, which is a mandatory input. Using the traces of the slices on 501s the detector a set of measurement windows is placed along these 501s traces. The data used for the determination of the gain and the 501s residual non-linearity is the taken from these windows. Bad pixels 501s indicated by an, optionally, provided bad pixel table, or flagged 501s during the preprocessing (bias subtraction) of the input data are 501s excluded from the measurements. Local measurements of the read-out- 501s noise, the signal and the gain are calculated for each of the 501s measurement windows. Using these measurements the gain for each 501s detector quadrant is computed as the zero-order coefficient of a 1st 501s order polynomial fitted to the binned gain measurements as a function 501s of the signal level. The residual non-linearity is modelled by a 501s (high) order polynomial which is fitted to the fractional percentage 501s deviation of the count rate from an expected constant count rate (the 501s linear case) as function of the signal level. (Not yet implemented!) 501s 501s Parameters: 501s nifu: IFU to handle. If set to 0, all IFUs are processed 501s serially. If set to -1, all IFUs are processed in 501s parallel. (int; default: 0) 501s ybox: Size of windows along the traces of the slices. (int; 501s default: 50) 501s xgap: Extra offset from tracing edge. (int; default: 3) 501s xborder: Extra offset from the detector edge used for the selection 501s of slices. (int; default: 10) 501s order: Order of the polynomial used to fit the non-linearity 501s residuals. (int; default: 12) 501s toffset: Exposure time offset in seconds to apply to linearity flat 501s fields. (float; default: 0.018) 501s fluxtol: Tolerance value for the overall flux consistency check of 501s a pair of flat fields. The value is the maximum relative 501s offset. (float; default: 0.01) 501s sigma: Sigma value used for signal value clipping. (float; 501s default: 3.0) 501s signalmin: Minimum signal value in log(ADU) used for the gain 501s analysis and the non-linearity polynomial model. (float; 501s default: 0.0) 501s signalmax: Maximum signal value in log(ADU) used for the gain 501s analysis and the non-linearity polynomial model. (float; 501s default: 4.9) 501s signalbin: Size of a signal bin in log10(ADU) used for the gain 501s analysis and the non-linearity polynomial model. (float; 501s default: 0.1) 501s gainlimit: Minimum signal value [ADU] used for fitting the gain 501s relation. (float; default: 100.0) 501s gainsigma: Sigma value for gain value clipping. (float; default: 3.0) 501s ctsmin: Minimum signal value in log(counts) to consider for the 501s non-linearity analysis. (float; default: 3.0) 501s ctsmax: Maximum signal value in log(counts) to consider for the 501s non-linearity analysis. (float; default: 4.9) 501s ctsbin: Size of a signal bin in log10(counts) used for the non- 501s linearity analysis. (float; default: 0.1) 501s linearmin: Lower limit of desired linear range in log10(counts). 501s (float; default: 2.5) 501s linearmax: Upper limit of desired linear range in log10(counts). 501s (float; default: 3.0) 501s merge: Merge output products from different IFUs into a common 501s file. (bool; default: False) 501s 501s Calibration frames: ['MASTER_BIAS', 'TRACE_TABLE', 'BADPIX_TABLE'] 501s 501s Raw and product frames: 501s LINGAIN_LAMP_OFF --> ['NONLINEARITY_GAIN'] 501s LINGAIN_LAMP_ON --> ['NONLINEARITY_GAIN'] 501s Author: Ralf Palsa 501s 501s 501s Recipe muse_dark: 501s version 2.8.7 501s 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} 501s Docstring: Combine several separate dark images into one master dark file and 501s locate hot pixels. 501s 501s This recipe combines several separate dark images into one master dark 501s file. The master dark contains the combined pixel values of the raw 501s dark exposures, with respect to the image combination method used and 501s normalization time specified. Processing trims the raw data and 501s records the overscan statistics, subtracts the bias (taking account of 501s the overscan, if --overscan is not "none") from each raw input image, 501s converts them from adu to count, scales them according to their 501s exposure time, and combines them using input parameters. Hot pixels 501s are then identified using image statistics and marked in the data 501s quality extension. The combined image is normalized to 1 hour exposure 501s time. QC statistics are computed on the output master dark. If 501s --model=true, a smooth polynomial model of the combined master dark is 501s computed, created from several individual 2D polynomials to describe 501s different features visible in MUSE dark frames. It is only advisable 501s to use this, if the master dark is the result of at least 50 501s individual long dark exposures. 501s 501s Parameters: 501s nifu: IFU to handle. If set to 0, all IFUs are processed 501s serially. If set to -1, all IFUs are processed in 501s parallel. (int; default: 0) 501s overscan: If this is "none", stop when detecting discrepant 501s overscan levels (see ovscsigma), for "offset" it assumes 501s that the mean overscan level represents the real offset 501s in the bias levels of the exposures involved, and adjusts 501s the data accordingly; for "vpoly", a polynomial is fit to 501s the vertical overscan and subtracted from the whole 501s quadrant. (str; default: 'vpoly') 501s ovscreject: This influences how values are rejected when computing 501s overscan statistics. Either no rejection at all ("none"), 501s rejection using the DCR algorithm ("dcr"), or rejection 501s using an iterative constant fit ("fit"). (str; default: 501s 'dcr') 501s ovscsigma: If the deviation of mean overscan levels between a raw 501s input image and the reference image is higher than 501s |ovscsigma x stdev|, stop the processing. If 501s overscan="vpoly", this is used as sigma rejection level 501s for the iterative polynomial fit (the level comparison is 501s then done afterwards with |100 x stdev| to guard against 501s incompatible settings). Has no effect for 501s overscan="offset". (float; default: 30.0) 501s ovscignore: The number of pixels of the overscan adjacent to the data 501s section of the CCD that are ignored when computing 501s statistics or fits. (int; default: 3) 501s combine: Type of image combination to use. (str; default: 501s 'sigclip') 501s nlow: Number of minimum pixels to reject with minmax. (int; 501s default: 1) 501s nhigh: Number of maximum pixels to reject with minmax. (int; 501s default: 1) 501s nkeep: Number of pixels to keep with minmax. (int; default: 1) 501s lsigma: Low sigma for pixel rejection with sigclip. (float; 501s default: 3.0) 501s hsigma: High sigma for pixel rejection with sigclip. (float; 501s default: 3.0) 501s scale: Scale the individual images to a common exposure time 501s before combining them. (bool; default: True) 501s normalize: Normalize the master dark to this exposure time (in 501s seconds). To disable normalization, set this to a 501s negative value. (float; default: 3600.0) 501s hotsigma: Sigma level, in terms of median deviation above the 501s median dark level, above which a pixel is detected and 501s marked as 'hot'. (float; default: 5.0) 501s model: Model the master dark using a set of polynomials. (bool; 501s default: False) 501s merge: Merge output products from different IFUs into a common 501s file. (bool; default: False) 501s 501s Calibration frames: ['MASTER_BIAS', 'BADPIX_TABLE'] 501s 501s Raw and product frames: 501s DARK --> ['MASTER_DARK', 'MODEL_DARK'] 501s Author: Peter Weilbacher 501s 501s 501s Recipe muse_bias: 501s version 2.8.7 501s 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} 501s Docstring: Combine several separate bias images into one master bias file. 501s 501s This recipe combines several separate bias images into one master bias 501s file. The master bias contains the combined pixel values, in adu, of 501s the raw bias exposures, with respect to the image combination method 501s used. Processing trims the raw data and records the overscan 501s statistics, corrects the data levels using the overscan (if overscan 501s is not "none") and combines the exposures using input parameters. The 501s read-out noise is computed for each quadrant of the raw input images 501s and stored as QC parameter. The variance extension is filled with an 501s initial value accordingly, before image combination. Further QC 501s statistics are computed on the output master bias. Additionally, bad 501s columns are searched for and marked in the data quality extension. 501s 501s Parameters: 501s nifu: IFU to handle. If set to 0, all IFUs are processed 501s serially. If set to -1, all IFUs are processed in 501s parallel. (int; default: 0) 501s overscan: If this is "none", stop when detecting discrepant 501s overscan levels (see ovscsigma), for "offset" it 501s assumes that the mean overscan level represents the 501s real offset in the bias levels of the exposures 501s involved, and adjusts the data accordingly; for 501s "vpoly", a polynomial is fit to the vertical overscan 501s and subtracted from the whole quadrant. (str; default: 501s 'vpoly') 501s ovscreject: This influences how values are rejected when computing 501s overscan statistics. Either no rejection at all 501s ("none"), rejection using the DCR algorithm ("dcr"), 501s or rejection using an iterative constant fit ("fit"). 501s (str; default: 'dcr') 501s ovscsigma: If the deviation of mean overscan levels between a raw 501s input image and the reference image is higher than 501s |ovscsigma x stdev|, stop the processing. If 501s overscan="vpoly", this is used as sigma rejection 501s level for the iterative polynomial fit (the level 501s comparison is then done afterwards with |100 x stdev| 501s to guard against incompatible settings). Has no effect 501s for overscan="offset". (float; default: 30.0) 501s ovscignore: The number of pixels of the overscan adjacent to the 501s data section of the CCD that are ignored when 501s computing statistics or fits. (int; default: 3) 501s combine: Type of image combination to use. (str; default: 501s 'sigclip') 501s nlow: Number of minimum pixels to reject with minmax. (int; 501s default: 1) 501s nhigh: Number of maximum pixels to reject with minmax. (int; 501s default: 1) 501s nkeep: Number of pixels to keep with minmax. (int; default: 501s 1) 501s lsigma: Low sigma for pixel rejection with sigclip. (float; 501s default: 3.0) 501s hsigma: High sigma for pixel rejection with sigclip. (float; 501s default: 3.0) 501s losigmabadpix: Low sigma to find dark columns in the combined bias 501s (float; default: 30.0) 501s hisigmabadpix: High sigma to find bright columns in the combined bias 501s (float; default: 3.0) 501s merge: Merge output products from different IFUs into a 501s common file. (bool; default: False) 501s 501s Calibration frames: ['BADPIX_TABLE'] 501s 501s Raw and product frames: 501s BIAS --> ['MASTER_BIAS'] 501s Author: Peter Weilbacher 501s 501s 501s Recipe muse_scipost_apply_astrometry: 501s version 2.8.7 501s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0} 501s Docstring: Calibrate astrometry for MUSE pixel tables. 501s 501s Apply an astrometric calibration to the pixel table spatial 501s coordinates. This is a task separated from muse_scipost. 501s 501s Parameters: 501s lambdamin: Cut off the data below this wavelength after loading the 501s pixel table(s). (float; default: 4000.0) 501s lambdamax: Cut off the data above this wavelength after loading the 501s pixel table(s). (float; default: 10000.0) 501s 501s Calibration frames: ['ASTROMETRY_WCS'] 501s 501s Raw and product frames: 501s PIXTABLE_OBJECT --> ['PIXTABLE_OBJECT'] 501s Author: Ole Streicher 501s 501s 501s Recipe muse_scipost_subtract_sky_simple: 501s version 2.8.7 501s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0} 501s Docstring: Subtract night sky spectrum. 501s 501s Subtract the sky in a simple way, just using a sky spectrum created by 501s muse_create_sky. This is a separated task of muse_scipost. 501s 501s Parameters: 501s lambdamin: Cut off the data below this wavelength after loading the 501s pixel table(s). (float; default: 4000.0) 501s lambdamax: Cut off the data above this wavelength after loading the 501s pixel table(s). (float; default: 10000.0) 501s 501s Calibration frames: ['SKY_SPECTRUM'] 501s 501s Raw and product frames: 501s PIXTABLE_REDUCED --> ['PIXTABLE_REDUCED'] 501s Author: Peter Weilbacher 501s 501s 501s Recipe muse_scipost_correct_dar: 501s version 2.8.7 501s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'lambdaref': 7000.0, 'darcheck': 'none'} 501s Docstring: Apply DAR correction for MUSE pixel tables. 501s 501s Correct the coordinates in the pixel table by differential atmospheric 501s refraction. This is a task separated from muse_scipost. 501s 501s Parameters: 501s lambdamin: Cut off the data below this wavelength after loading the 501s pixel table(s). (float; default: 4000.0) 501s lambdamax: Cut off the data above this wavelength after loading the 501s pixel table(s). (float; default: 10000.0) 501s lambdaref: Reference wavelength used for correction of differential 501s atmospheric refraction. The R-band (peak wavelength ~7000 501s Angstrom) that is usually used for guiding, is close to 501s the central wavelength of MUSE, so a value of 7000.0 501s Angstrom should be used if nothing else is known. A value 501s less than zero switches DAR correction off. (float; 501s default: 7000.0) 501s darcheck: Carry out a check of the theoretical DAR correction using 501s source centroiding. If "correct" it will also apply an 501s empirical correction. (str; default: 'none') 501s 501s Calibration frames: [] 501s 501s Raw and product frames: 501s PIXTABLE_OBJECT --> ['PIXTABLE_OBJECT'] 501s Author: Ole Streicher 501s 501s 501s Recipe muse_scipost_correct_rv: 501s version 2.8.7 501s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'rvcorr': 'bary'} 501s Docstring: Apply RV correction for MUSE pixel tables. 501s 501s Correct the wavelengths in the pixel table by given radial-velocity 501s correction. This is a task separated from muse_scipost. 501s 501s Parameters: 501s lambdamin: Cut off the data below this wavelength after loading the 501s pixel table(s). (float; default: 4000.0) 501s lambdamax: Cut off the data above this wavelength after loading the 501s pixel table(s). (float; default: 10000.0) 501s rvcorr: Correct the radial velocity of the telescope with 501s reference to either the barycenter of the Solar System 501s (bary), the center of the Sun (helio), or to the center of 501s the Earth (geo). (str; default: 'bary') 501s 501s Calibration frames: [] 501s 501s Raw and product frames: 501s PIXTABLE_OBJECT --> ['PIXTABLE_REDUCED'] 501s Author: Peter Weilbacher 501s 501s 501s Recipe muse_exp_align: 501s version 2.8.7 501s 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} 501s Docstring: Create a coordinate offset table to be used to align exposures during 501s exposure combination. 501s 501s Compute the coordinate offset for each input field-of-view image with 501s respect to a reference. The created list of coordinate offsets can 501s then be used in muse_exp_combine as the field coordinate offsets to 501s properly align the exposures during their combination. The source 501s positions used to compute the field offsets are obtained by detecting 501s point sources in each of the input images, unless the source detection 501s is overridden and an input source list is available for each input 501s field-of-view image. In this latter case the input source positions 501s are used to calculate the field offsets. 501s 501s Parameters: 501s rsearch: Search radius (in arcsec) for each iteration of 501s the offset computation. (str; default: 501s '30.,4.,2.,0.8') 501s nbins: Number of bins to use for 2D histogram on the 501s first iteration of the offset computation. (int; 501s default: 60) 501s weight: Use weighting. (bool; default: True) 501s fwhm: FWHM in pixels of the convolution filter. (float; 501s default: 5.0) 501s threshold: Initial intensity threshold for detecting point 501s sources. If the value is negative or zero the 501s threshold is taken as sigma above median 501s background MAD. If it is larger than zero the 501s threshold is taken as absolute background level. 501s (float; default: 15.0) 501s bkgignore: Fraction of the image to be ignored. (float; 501s default: 0.05) 501s bkgfraction: Fraction of the image (without the ignored part) 501s to be considered as background. (float; default: 501s 0.1) 501s step: Increment/decrement of the threshold value in 501s subsequent iterations. (float; default: 0.5) 501s iterations: Maximum number of iterations used for detecting 501s sources. (int; default: 100000) 501s srcmin: Minimum number of sources which must be found. 501s (int; default: 5) 501s srcmax: Maximum number of sources which may be found. 501s (int; default: 80) 501s roundmin: Lower limit of the allowed point-source 501s roundness. (float; default: -1.0) 501s roundmax: Upper limit of the allowed point-source 501s roundness. (float; default: 1.0) 501s sharpmin: Lower limit of the allowed point-source 501s sharpness. (float; default: 0.2) 501s sharpmax: Upper limit of the allowed point-source 501s sharpness. (float; default: 1.0) 501s expmap: Enables the creation of a simple exposure map for 501s the combined field- of-view. (bool; default: 501s False) 501s bpixdistance: Minimum allowed distance of a source to the 501s closest bad pixel in pixel. Detected sources 501s which are closer to a bad pixel are not taken 501s into account when computing the field offsets. 501s This option has no effect if the source positions 501s are taken from input catalogs. (float; default: 501s 5.0) 501s override_detection: Overrides the source detection step. If this is 501s enabled and source catalogs are present in the 501s input data set, the source positions used to 501s calculate the field offsets are read from the 501s input catalogs. If no catalogs are available as 501s input data the source positions are detected on 501s the input images. (bool; default: False) 501s 501s Calibration frames: ['SOURCE_LIST'] 501s 501s Raw and product frames: 501s IMAGE_FOV --> ['EXPOSURE_MAP', 'PREVIEW_FOV', 'SOURCE_LIST', 501s 'OFFSET_LIST'] 501s Author: Ralf Palsa 501s 501s 501s Recipe muse_scipost: 501s version 2.8.7 501s 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} 501s Docstring: Prepare reduced and combined science products. 501s 501s Sort input pixel tables into lists of files per exposure, merge pixel 501s tables from all IFUs of each exposure. Correct each exposure for 501s differential atmospheric refraction (unless --lambdaref is far outside 501s the MUSE wavelength range, or NFM is used which has a built-in 501s corrector). Then the flux calibration is carried out, if a response 501s curve was given in the input; it includes a correction of telluric 501s absorption, if a telluric absorption correction file was given. If 501s observations were done with AO and a RAMAN_LINES file was given, a 501s procedure is run to clean the Raman scattering emission lines from the 501s data. Next, the slice autocalibration is computed and the flux 501s correction factors are applied to the pixel table (if 501s --autocalib="deepfield"). If user-provided autocalibration is 501s requested (--autocalib="user"), then the autocalibration is not 501s computed on the input exposure but the autocalibration factors are 501s read from the AUTOCAL_FACTORS table and applied directly to the data. 501s Then the sky subtraction is carried out (unless --skymethod="none"), 501s either directly subtracting an input sky continuum and an input sky 501s emission lines (for --skymethod="subtract-model"), or 501s (--skymethod="model") create a sky spectrum from the darkest fraction 501s (--skymodel_fraction, after ignoring the lowest --skymodel_ignore as 501s artifacts) of the field of view, then fitting and subtracting sky 501s emission lines using an initial estimate of the input sky lines; then 501s the continuum (residuals after subtracting the sky lines from the sky 501s spectrum) is subtracted as well. If --save contains "skymodel", all 501s sky-related products are saved for each exposure. Afterwards the data 501s is corrected for the radial velocity of the observer (--rvcorr), 501s before the input (or a default) astrometric solution is applied. Now 501s each individual exposure is fully reduced; the pixel tables at this 501s stage can be saved by setting "individual" in --save. If multiple 501s exposures were given, they are then combined. If --save contains 501s "combined", this final merged pixel table is saved. Finally (if --save 501s contains "cube"), the data is resampled into a datacube, using all 501s parameters given to the recipe. The extent and orientation of the cube 501s is normally computed from the data itself, but this can be overridden 501s by passing a file with the output world coordinate system 501s (OUTPUT_WCS), for example a MUSE cube. This can also be used to sample 501s the wavelength axis logarithmically (in that file set "CTYPE3='AWAV- 501s LOG'"). As a last step, the computed cube is integrated over all 501s filter functions given (--filter) that are also present in the input 501s filter list table. 501s 501s Parameters: 501s save: Select output product(s) to save. Can contain one 501s or more of "cube", "autocal", "skymodel", 501s "individual", "positioned", "combined", and 501s "stacked". If several options are given, they 501s have to be comma- separated. ("cube": output cube 501s and associated images, if this is not given, no 501s final resampling is done at all -- "autocal": up 501s to two additional output products related to the 501s slice autocalibration -- "raman": up to four 501s additional output products about the Raman light 501s distribution for AO observations -- "skymodel": 501s up to four additional output products about the 501s effectively used sky that was subtracted with the 501s "model" method -- "individual": fully reduced 501s pixel table for each individual exposure -- 501s "positioned": fully reduced and positioned pixel 501s table for each individual exposure, the 501s difference to "individual" is that here, the 501s output pixel tables have coordinates in RA and 501s DEC, and the optional offsets were applied; this 501s is only useful, if both the relative exposure 501s weighting and the final resampling are to be done 501s externally -- "combined": fully reduced and 501s combined pixel table for the full set of 501s exposures, the difference to "positioned" is that 501s all pixel tables are combined into one, with an 501s added weight column; this is useful, if only the 501s final resampling step is to be done separately -- 501s "stacked": an additional output file in form of a 501s 2D column-stacked image, i.e. x direction is 501s pseudo-spatial, y direction is wavelength.) (str; 501s default: 'cube,skymodel') 501s resample: The resampling technique to use for the final 501s output cube. (str; default: 'drizzle') 501s dx: Horizontal step size for resampling (in arcsec or 501s pixel). The following defaults are taken when 501s this value is set to 0.0: 0.2'' for WFM, 0.025'' 501s for NFM, 1.0 if data is in pixel units. (float; 501s default: 0.0) 501s dy: Vertical step size for resampling (in arcsec or 501s pixel). The following defaults are taken when 501s this value is set to 0.0: 0.2'' for WFM, 0.025'' 501s for NFM, 1.0 if data is in pixel units. (float; 501s default: 0.0) 501s dlambda: Wavelength step size (in Angstrom). Natural 501s instrument sampling is used, if this is 0.0 501s (float; default: 0.0) 501s crtype: Type of statistics used for detection of cosmic 501s rays during final resampling. "iraf" uses the 501s variance information, "mean" uses standard 501s (mean/stdev) statistics, "median" uses median and 501s the median median of the absolute median 501s deviation. (str; default: 'median') 501s crsigma: Sigma rejection factor to use for cosmic ray 501s rejection during final resampling. A zero or 501s negative value switches cosmic ray rejection off. 501s (float; default: 15.0) 501s rc: Critical radius for the "renka" resampling 501s method. (float; default: 1.25) 501s pixfrac: Pixel down-scaling factor for the "drizzle" 501s resampling method. Up to three, comma-separated, 501s floating-point values can be given. If only one 501s value is given, it applies to all dimensions, two 501s values are interpreted as spatial and spectral 501s direction, respectively, while three are taken as 501s horizontal, vertical, and spectral. (str; 501s default: '0.8,0.8') 501s ld: Number of adjacent pixels to take into account 501s during resampling in all three directions (loop 501s distance); this affects all resampling methods 501s except "nearest". (int; default: 1) 501s format: Type of output file format, "Cube" is a standard 501s FITS cube with NAXIS=3 and multiple extensions 501s (for data and variance). The extended "x" formats 501s include the reconstructed image(s) in FITS image 501s extensions within the same file. "sdpCube" does 501s some extra calculations to create FITS keywords 501s for the ESO Science Data Products. (str; default: 501s 'Cube') 501s weight: Type of weighting scheme to use when combining 501s multiple exposures. "exptime" just uses the 501s exposure time to weight the exposures, "fwhm" 501s uses the best available seeing information from 501s the headers as well, "none" preserves an existing 501s weight column in the input pixel tables without 501s changes. (str; default: 'exptime') 501s filter: The filter name(s) to be used for the output 501s field-of-view image. Each name has to correspond 501s to an EXTNAME in an extension of the FILTER_LIST 501s file. If an unsupported filter name is given, 501s creation of the respective image is omitted. If 501s multiple filter names are given, they have to be 501s comma separated. (str; default: 'white') 501s autocalib: The type of autocalibration to use. "none" 501s switches it off, "deepfield" uses the revised 501s MPDAF method that can be used for the reduction 501s of mostly empty "Deep Fields", "user" searches 501s for a user- provided table with autocalibration 501s factors. (str; default: 'none') 501s raman_width: Wavelength range around Raman lines [Angstrom]. 501s (float; default: 20.0) 501s skymethod: The method used to subtract the sky background 501s (spectrum). Option "model" should work in all 501s kinds of science fields: it uses a global sky 501s spectrum model with a local LSF. "model" uses 501s fluxes indicated in the SKY_LINES file as 501s starting estimates, but re-fits them on the 501s global sky spectrum created from the science 501s exposure. If SKY_CONTINUUM is given, it is 501s directly subtracted, otherwise it is created from 501s the sky region of the science exposure. Option 501s "subtract- model" uses the input SKY_LINES and 501s SKY_CONTINUUM, subtracting them directly without 501s re-fitting the fluxes, but still makes use of the 501s local LSF, hence LSF_PROFILE is required. The 501s inputs LSF_PROFILE and SKY_LINES are necessary 501s for these two model-based methods; SKY_CONTINUUM 501s is required for "subtract-model" and optional for 501s "model"; SKY_MASK is optional for "model". 501s Finally, option "simple" creates a sky spectrum 501s from the science data, and directly subtracts it, 501s without taking the LSF into account (LSF_PROFILE 501s and input SKY files are ignored). It works on 501s data that was not flux calibrated. (str; default: 501s 'model') 501s lambdamin: Cut off the data below this wavelength after 501s loading the pixel table(s). (float; default: 501s 4000.0) 501s lambdamax: Cut off the data above this wavelength after 501s loading the pixel table(s). (float; default: 501s 10000.0) 501s lambdaref: Reference wavelength used for correction of 501s differential atmospheric refraction. The R-band 501s (peak wavelength ~7000 Angstrom) that is usually 501s used for guiding, is close to the central 501s wavelength of MUSE, so a value of 7000.0 Angstrom 501s should be used if nothing else is known. A value 501s less than zero switches DAR correction off. 501s (float; default: 7000.0) 501s darcheck: Carry out a check of the theoretical DAR 501s correction using source centroiding. If "correct" 501s it will also apply an empirical correction. (str; 501s default: 'none') 501s skymodel_fraction: Fraction of the image (without the ignored part) 501s to be considered as sky. If an input sky mask is 501s provided, the fraction is applied to the regions 501s within the mask. If the whole sky mask should be 501s used, set this parameter to 1. (float; default: 501s 0.1) 501s skymodel_ignore: Fraction of the image to be ignored. If an input 501s sky mask is provided, the fraction is applied to 501s the regions within the mask. If the whole sky 501s mask should be used, set this parameter to 0. 501s (float; default: 0.05) 501s skymodel_sampling: Spectral sampling of the sky spectrum [Angstrom]. 501s (float; default: 0.3125) 501s skymodel_csampling: Spectral sampling of the continuum spectrum 501s [Angstrom]. (float; default: 0.3125) 501s sky_crsigma: Sigma level clipping for cube-based and spectrum- 501s based CR rejection when creating the sky 501s spectrum. This has to be a string of two comma- 501s separated floating-point numbers. The first value 501s gives the sigma- level rejection for cube-based 501s CR rejection (using "median"), the second value 501s the sigma-level for spectrum-based CR cleaning. 501s Both can be switched off, by passing zero or a 501s negative value. (str; default: '15.,15.') 501s rvcorr: Correct the radial velocity of the telescope with 501s reference to either the barycenter of the Solar 501s System (bary), the center of the Sun (helio), or 501s to the center of the Earth (geo). (str; default: 501s 'bary') 501s astrometry: If false, skip any astrometric calibration, even 501s if one was passed in the input set of files. This 501s causes creation of an output cube with a linear 501s WCS and may result in errors. If you want to use 501s a sensible default, leave this true but do not 501s pass an ASTROMETRY_WCS. (bool; default: True) 501s 501s Calibration frames: ['EXTINCT_TABLE', 'STD_RESPONSE', 'STD_TELLURIC', 501s 'ASTROMETRY_WCS', 'OFFSET_LIST', 'FILTER_LIST', 501s 'OUTPUT_WCS', 'AUTOCAL_FACTORS', 'RAMAN_LINES', 501s 'SKY_LINES', 'SKY_CONTINUUM', 'LSF_PROFILE', 501s 'SKY_MASK'] 501s 501s Raw and product frames: 501s PIXTABLE_OBJECT --> ['DATACUBE_FINAL', 'IMAGE_FOV', 501s 'OBJECT_RESAMPLED', 'PIXTABLE_REDUCED', 501s 'PIXTABLE_POSITIONED', 'PIXTABLE_COMBINED', 501s 'AUTOCAL_MASK', 'AUTOCAL_FACTORS', 501s 'RAMAN_IMAGES', 'SKY_IMAGE', 'SKY_MASK', 501s 'SKY_SPECTRUM', 'SKY_LINES', 'SKY_CONTINUUM'] 501s Author: Peter Weilbacher 501s 501s 501s Recipe muse_scipost_calibrate_flux: 501s version 2.8.7 501s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0} 501s Docstring: Calibrate flux for MUSE pixel tables. 501s 501s Replace the intensity in the MUSE pixel tables by the absolute flux. 501s This is a task separated from muse_scipost. 501s 501s Parameters: 501s lambdamin: Cut off the data below this wavelength after loading the 501s pixel table(s). (float; default: 4000.0) 501s lambdamax: Cut off the data above this wavelength after loading the 501s pixel table(s). (float; default: 10000.0) 501s 501s Calibration frames: ['EXTINCT_TABLE', 'STD_RESPONSE', 'STD_TELLURIC'] 501s 501s Raw and product frames: 501s PIXTABLE_OBJECT --> ['PIXTABLE_OBJECT'] 501s Author: Ole Streicher 501s 501s 501s Recipe muse_flat: 501s version 2.8.7 501s 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} 501s Docstring: Combine several separate flat images into one master flat file, trace 501s slice locations, and locate dark pixels. 501s 501s This recipe combines several separate flat-field images into one 501s master flat-field file and traces the location of the slices on the 501s CCD. The master flat contains the combined pixel values of the raw 501s flat exposures, with respect to the image combination method used, 501s normalized to the mean flux. The trace table contains polynomials 501s defining the location of the slices on the CCD. Processing trims the 501s raw data and records the overscan statistics, subtracts the bias 501s (taking account of the overscan, if --overscan is not "none"), and 501s optionally, the dark from each raw input image, converts them from adu 501s to count, scales them according to their exposure time, and combines 501s the exposures using input parameters. To trace the position of the 501s slices on the CCD, their edges are located using a threshold method. 501s The edge detection is repeated at given intervals thereby tracing the 501s central position (the mean of both edges) and width of each slit 501s vertically across the CCD. Deviant positions of detections on CCD rows 501s can be detected and excluded before fitting a polynomial to all 501s positions measured for one slice. The polynomial parameters for each 501s slice are saved in the output trace table. Finally, the area between 501s the now known slice edges is searched for dark (and bright) pixels, 501s using statistics in each row of the master flat. 501s 501s Parameters: 501s nifu: IFU to handle. If set to 0, all IFUs are processed 501s serially. If set to -1, all IFUs are processed in 501s parallel. (int; default: 0) 501s overscan: If this is "none", stop when detecting discrepant 501s overscan levels (see ovscsigma), for "offset" it 501s assumes that the mean overscan level represents the 501s real offset in the bias levels of the exposures 501s involved, and adjusts the data accordingly; for 501s "vpoly", a polynomial is fit to the vertical overscan 501s and subtracted from the whole quadrant. (str; default: 501s 'vpoly') 501s ovscreject: This influences how values are rejected when computing 501s overscan statistics. Either no rejection at all 501s ("none"), rejection using the DCR algorithm ("dcr"), 501s or rejection using an iterative constant fit ("fit"). 501s (str; default: 'dcr') 501s ovscsigma: If the deviation of mean overscan levels between a raw 501s input image and the reference image is higher than 501s |ovscsigma x stdev|, stop the processing. If 501s overscan="vpoly", this is used as sigma rejection 501s level for the iterative polynomial fit (the level 501s comparison is then done afterwards with |100 x stdev| 501s to guard against incompatible settings). Has no effect 501s for overscan="offset". (float; default: 30.0) 501s ovscignore: The number of pixels of the overscan adjacent to the 501s data section of the CCD that are ignored when 501s computing statistics or fits. (int; default: 3) 501s combine: Type of combination to use (str; default: 'sigclip') 501s nlow: Number of minimum pixels to reject with minmax (int; 501s default: 1) 501s nhigh: Number of maximum pixels to reject with minmax (int; 501s default: 1) 501s nkeep: Number of pixels to keep with minmax (int; default: 1) 501s lsigma: Low sigma for pixel rejection with sigclip (float; 501s default: 3.0) 501s hsigma: High sigma for pixel rejection with sigclip (float; 501s default: 3.0) 501s scale: Scale the individual images to a common exposure time 501s before combining them. (bool; default: True) 501s normalize: Normalize the master flat to the average flux (bool; 501s default: True) 501s trace: Trace the position of the slices on the master flat 501s (bool; default: True) 501s nsum: Number of lines over which to average when tracing 501s (int; default: 32) 501s order: Order of polynomial fit to the trace (int; default: 5) 501s edgefrac: Fractional change required to identify edge when 501s tracing (float; default: 0.5) 501s losigmabadpix: Low sigma to find dark pixels in the master flat 501s (float; default: 5.0) 501s hisigmabadpix: High sigma to find bright pixels in the master flat 501s (float; default: 5.0) 501s samples: Create a table containing all tracing sample points. 501s (bool; default: False) 501s merge: Merge output products from different IFUs into a 501s common file. (bool; default: False) 501s 501s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'BADPIX_TABLE'] 501s 501s Raw and product frames: 501s FLAT --> ['MASTER_FLAT', 'TRACE_TABLE', 'TRACE_SAMPLES'] 501s Author: Peter Weilbacher (based on Joris Gerssen's draft) 501s 501s 501s Recipe muse_wavecal: 501s version 2.8.7 501s 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} 501s Docstring: Detect arc emission lines and determine the wavelength solution for 501s each slice. 501s 501s This recipe detects arc emission lines and fits a wavelength solution 501s to each slice of the instrument. The wavelength calibration table 501s contains polynomials defining the wavelength solution of the slices on 501s the CCD. Processing trims the raw data and records the overscan 501s statistics, subtracts the bias (taking account of the overscan, if 501s --overscan is not "none") and converts them from adu to count. 501s Optionally, the dark can be subtracted and the data can be divided by 501s the flat-field, but this is not recommended. The data is then combined 501s using input parameters, into separate images for each lamp. To compute 501s the wavelength solution, arc lines are detected at the center of each 501s slice (using threshold detection on a S/N image) and subsequently 501s assigned wavelengths, using pattern matching to identify lines from 501s the input line catalog. Each line is then traced to the edges of the 501s slice, using Gaussian centering in each CCD column. The Gaussians not 501s only yield center, but also centering error, and line properties (e.g. 501s FWHM). Deviant fits are detected using polynomial fits to each arc 501s line (using the xorder parameter) and rejected. These analysis and 501s measuring steps are carried out separately on images exposed by the 501s different arc lamps, reducing the amount of blending, that can 501s otherwise influence line identification and Gaussian centering. The 501s final two-dimensional fit uses all positions (of all lamps), their 501s wavelengths, and the given polynomial orders to compute the final 501s wavelength solution for each slice, iteratively rejecting outliers. 501s This final fit can be either unweighted (fitweighting="uniform", for 501s fastest processing) or weighted (other values of fitweighting, for 501s higher accuracy). 501s 501s Parameters: 501s nifu: IFU to handle. If set to 0, all IFUs are processed 501s serially. If set to -1, all IFUs are processed in 501s parallel. (int; default: 0) 501s overscan: If this is "none", stop when detecting discrepant 501s overscan levels (see ovscsigma), for "offset" it 501s assumes that the mean overscan level represents the 501s real offset in the bias levels of the exposures 501s involved, and adjusts the data accordingly; for 501s "vpoly", a polynomial is fit to the vertical overscan 501s and subtracted from the whole quadrant. (str; default: 501s 'vpoly') 501s ovscreject: This influences how values are rejected when computing 501s overscan statistics. Either no rejection at all 501s ("none"), rejection using the DCR algorithm ("dcr"), or 501s rejection using an iterative constant fit ("fit"). 501s (str; default: 'dcr') 501s ovscsigma: If the deviation of mean overscan levels between a raw 501s input image and the reference image is higher than 501s |ovscsigma x stdev|, stop the processing. If 501s overscan="vpoly", this is used as sigma rejection level 501s for the iterative polynomial fit (the level comparison 501s is then done afterwards with |100 x stdev| to guard 501s against incompatible settings). Has no effect for 501s overscan="offset". (float; default: 30.0) 501s ovscignore: The number of pixels of the overscan adjacent to the 501s data section of the CCD that are ignored when computing 501s statistics or fits. (int; default: 3) 501s combine: Type of lampwise image combination to use. (str; 501s default: 'sigclip') 501s lampwise: Identify and measure the arc emission lines on images 501s separately for each lamp setup. (bool; default: True) 501s sigma: Sigma level used to detect arc emission lines above the 501s median background level in the S/N image of the central 501s column of each slice (float; default: 1.0) 501s dres: The allowed range of resolutions for pattern matching 501s (of detected arc lines to line list) in fractions 501s relative to the expected value (float; default: 0.05) 501s tolerance: Tolerance for pattern matching (of detected arc lines 501s to line list) (float; default: 0.1) 501s xorder: Order of the polynomial for the horizontal curvature 501s within each slice (int; default: 2) 501s yorder: Order of the polynomial used to fit the dispersion 501s relation (int; default: 6) 501s linesigma: Sigma level for iterative rejection of deviant fits for 501s each arc line within each slice, a negative value means 501s to use the default (2.5). (float; default: -1.0) 501s residuals: Create a table containing residuals of the fits to the 501s data of all arc lines. This is useful to assess the 501s quality of the wavelength solution in detail. (bool; 501s default: False) 501s fitsigma: Sigma level for iterative rejection of deviant 501s datapoints during the final polynomial wavelength 501s solution within each slice, a negative value means to 501s use the default (3.0). (float; default: -1.0) 501s fitweighting: Type of weighting to use in the final polynomial 501s wavelength solution fit, using centroiding error 501s estimate and/or scatter of each single line as 501s estimates of its accuracy. (str; default: 501s 'cerrscatter') 501s saveimages: Save (bool; default: False) 501s resample: Resample the input arc images onto 2D images for a 501s visual check using tracing and wavelength calibration 501s solutions. Note that the image produced will show small 501s wiggles even when the calibration was successful! 501s (bool; default: False) 501s wavemap: Create a wavelength map of the input images (bool; 501s default: False) 501s merge: Merge output products from different IFUs into a common 501s file. (bool; default: False) 501s 501s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 501s 'TRACE_TABLE', 'LINE_CATALOG', 'BADPIX_TABLE'] 501s 501s Raw and product frames: 501s ARC --> ['WAVECAL_TABLE', 'WAVECAL_RESIDUALS', 'ARC_RED_LAMP'] 501s Author: Peter Weilbacher 501s 501s 501s Recipe muse_twilight: 501s version 2.8.7 501s 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} 501s Docstring: Combine several twilight skyflats into one cube, compute correction 501s factors for each IFU, and create a smooth 3D illumination correction. 501s 501s Processing first handles each raw input image separately: it trims the 501s raw data and records the overscan statistics, subtracts the bias 501s (taking account of the overscan, if --overscan is not "none"), 501s converts the images from adu to count, subtracts the dark, divides by 501s the flat-field and combines all the exposures using input parameters. 501s The input calibrations geometry table, trace table, and wavelength 501s calibration table are used to assign 3D coordinates to each CCD-based 501s pixel, thereby creating a pixel table from the master sky-flat. These 501s pixel tables are then cut in wavelength using the --lambdamin and 501s --lambdamax parameters. The integrated flux in each IFU is computed as 501s the sum of the data in the pixel table, and saved in the header, to be 501s used later as estimate for the relative throughput of each IFU. If an 501s ILLUM exposure was given as input, it is then used to correct the 501s relative illumination between all slices of one IFU. For this, the 501s data of each slice within the pixel table of each IFU is multiplied by 501s the normalized median flux of that slice in the ILLUM exposure. The 501s pixel tables of all IFUs are then merged, using the integrated fluxes 501s as inverse scaling factors, and a cube is reconstructed from the 501s merged dataset, using given parameters. A white-light image is created 501s from the cube. This skyflat cube is then saved to disk, with the 501s white-light image as one extension. To construct a smooth 3D 501s illumination correction, the cube is post-processed in the following 501s way: the white-light image is used to create a mask of the illuminated 501s area. From this area, the optional vignetting mask is removed. The 501s smoothing is then computed for each plane of the cube: the illuminated 501s area is smoothed (by a 5x7 median filter), normalized, fit with a 2D 501s polynomial (of given polynomial orders), and normalized again. A 501s smooth white image is then created by collapsing the smooth cube. If a 501s vignetting mask was given or NFM data is processed, an area close to 501s the edge of the MUSE field is used to compute a 2D correction for the 501s vignetted area: the original unsmoothed white-light image is corrected 501s for large scale gradients by dividing it with the smooth white image. 501s The residuals in the edge area (as defined by the input mask or 501s hardcoded for NFM) are then smoothed using input parameters. This 501s smoothed vignetting correction is the multiplied onto each plane of 501s the smooth cube, normalizing each plane again. This twilight cube is 501s then saved to disk. 501s 501s Parameters: 501s overscan: If this is "none", stop when detecting discrepant 501s overscan levels (see ovscsigma), for "offset" it 501s assumes that the mean overscan level represents the 501s real offset in the bias levels of the exposures 501s involved, and adjusts the data accordingly; for 501s "vpoly", a polynomial is fit to the vertical overscan 501s and subtracted from the whole quadrant. (str; default: 501s 'vpoly') 501s ovscreject: This influences how values are rejected when computing 501s overscan statistics. Either no rejection at all 501s ("none"), rejection using the DCR algorithm ("dcr"), 501s or rejection using an iterative constant fit ("fit"). 501s (str; default: 'dcr') 501s ovscsigma: If the deviation of mean overscan levels between a raw 501s input image and the reference image is higher than 501s |ovscsigma x stdev|, stop the processing. If 501s overscan="vpoly", this is used as sigma rejection 501s level for the iterative polynomial fit (the level 501s comparison is then done afterwards with |100 x stdev| 501s to guard against incompatible settings). Has no effect 501s for overscan="offset". (float; default: 30.0) 501s ovscignore: The number of pixels of the overscan adjacent to the 501s data section of the CCD that are ignored when 501s computing statistics or fits. (int; default: 3) 501s combine: Type of combination to use (str; default: 'sigclip') 501s nlow: Number of minimum pixels to reject with minmax (int; 501s default: 1) 501s nhigh: Number of maximum pixels to reject with minmax (int; 501s default: 1) 501s nkeep: Number of pixels to keep with minmax (int; default: 1) 501s lsigma: Low sigma for pixel rejection with sigclip (float; 501s default: 3.0) 501s hsigma: High sigma for pixel rejection with sigclip (float; 501s default: 3.0) 501s scale: Scale the individual images to a common exposure time 501s before combining them. (bool; default: False) 501s resample: The resampling technique to use for the final output 501s cube. (str; default: 'drizzle') 501s crtype: Type of statistics used for detection of cosmic rays 501s during final resampling. "iraf" uses the variance 501s information, "mean" uses standard (mean/stdev) 501s statistics, "median" uses median and the median median 501s of the absolute median deviation. (str; default: 501s 'median') 501s crsigma: Sigma rejection factor to use for cosmic ray rejection 501s during final resampling. A zero or negative value 501s switches cosmic ray rejection off. (float; default: 501s 50.0) 501s lambdamin: Minimum wavelength for twilight reconstruction. 501s (float; default: 5000.0) 501s lambdamax: Maximum wavelength for twilight reconstruction. 501s (float; default: 9000.0) 501s dlambda: Sampling for twilight reconstruction, this should 501s result in planes of equal wavelength coverage. (float; 501s default: 250.0) 501s xorder: Polynomial order to use in x direction to fit the full 501s field of view. (int; default: 2) 501s yorder: Polynomial order to use in y direction to fit the full 501s field of view. (int; default: 2) 501s vignmaskedges: Pixels on edges stronger than this fraction in the 501s normalized image are excluded from the fit to the 501s vignetted area. Set to non-positive number to include 501s them in the fit. This has no effect for NFM skyflats. 501s (float; default: 0.02) 501s vignsmooth: Type of smoothing to use for the vignetted region 501s given by the VIGNETTING_MASK (for WFM, or the internal 501s mask, for NFM); gaussian uses (vignxpar + vignypar)/2 501s as FWHM. (str; default: 'polyfit') 501s vignxpar: Parameter used by the vignetting smoothing: x order 501s for polyfit (default, recommended 4), parameter that 501s influences the FWHM for the gaussian (recommended: 501s 10), or x dimension of median filter (recommended 5). 501s If a negative value is found, the default is taken. 501s (int; default: -1) 501s vignypar: Parameter used by the vignetting smoothing: y order 501s for polyfit (default, recommended 4), parameter that 501s influences the FWHM for the gaussian (recommended: 501s 10), or y dimension of median filter (recommended 5). 501s If a negative value is found, the default is taken. 501s (int; default: -1) 501s vignnfmmask: The height of the vignetted region at the top of the 501s MUSE field in NFM. This is the region modeled 501s separately (the final vignetting model might be 501s smaller). (int; default: 22) 501s 501s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 501s 'BADPIX_TABLE', 'TRACE_TABLE', 'WAVECAL_TABLE', 501s 'GEOMETRY_TABLE', 'VIGNETTING_MASK'] 501s 501s Raw and product frames: 501s SKYFLAT --> ['DATACUBE_SKYFLAT', 'TWILIGHT_CUBE'] 501s ILLUM --> [] 501s Author: Peter Weilbacher 501s 501s 501s Recipe muse_qi_mask: 501s version 2.8.7 501s Parameters: {'nifu': 0} 501s Docstring: Create image masks for use with the quick image reconstruction. 501s 501s Trace and wavelength calibration tables (24 of them each, one per IFU) 501s are used to build wavelength maps. If the input data is binned, the 501s wavelength maps are binned in the same way (averaging of pixels). The 501s wavelength maps are then thresholded to create masks of the desired 501s wavelength range. Finally, the mask is "untrimmed", i.e. empty regions 501s for the pre- and overscans are added (in a simple way, assuming 501s quadrants of equal size, and padding of 32 pixels on all quadrant 501s edges). Note: this recipe is not part of the main MUSE pipeline but to 501s be used in the integration phase to create image masks until the 501s system is fully qualified. It therefore does only minimal error 501s checking. 501s 501s Parameters: 501s nifu: IFU to handle. If set to 0, all IFUs are processed serially, 501s which is the recommendation for this recipe, since only then 501s all extensions end up in the same output file. (int; default: 501s 0) 501s 501s Calibration frames: ['TRACE_TABLE', 'WAVECAL_TABLE'] 501s 501s Raw and product frames: 501s BIAS --> ['MASK_IMAGE'] 501s Author: Peter Weilbacher 501s 501s 501s Recipe muse_ampl: 501s version 2.8.7 501s 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} 501s Docstring: Determine the instrumental throughput from exposures taken with the 501s pico-amplifier / photo diode readings. 501s 501s This recipe combines several separate amplifier images (flat-fields 501s with special FITS headers containing pico amplifier measurements) into 501s one master image file and computes the instrumental throughput per IFU 501s (and slice). Processing trims the raw data and records the overscan 501s statistics, subtracts the bias (taking account of the overscan, if 501s overscan is not "none"), and optionally, the dark from each raw input 501s image, converts them from adu to count, scales them according to their 501s exposure time, and combines them using input parameters. To compute 501s the throughput the image is converted into a pixel table, the flux is 501s then integrated over the given filter band, and the ratio of the 501s expected flux (FITS header INS.AMPL2.CURR) to measured flux is taken, 501s in the same units. If a geometry table was given as input, the 501s relative area of the IFUs is taken into account when computing the 501s flux per unit area. The resulting ratio is the instrument efficiency 501s (throughput) and saved as QC parameters for the whole input image and 501s per slice in the output pixel table. 501s 501s Parameters: 501s nifu: IFU to handle. If set to 0, all IFUs are processed 501s serially. If set to -1, all IFUs are processed in 501s parallel. (int; default: 0) 501s overscan: If this is "none", stop when detecting discrepant 501s overscan levels (see ovscsigma), for "offset" it assumes 501s that the mean overscan level represents the real offset 501s in the bias levels of the exposures involved, and adjusts 501s the data accordingly; for "vpoly", a polynomial is fit to 501s the vertical overscan and subtracted from the whole 501s quadrant. (str; default: 'vpoly') 501s ovscreject: This influences how values are rejected when computing 501s overscan statistics. Either no rejection at all ("none"), 501s rejection using the DCR algorithm ("dcr"), or rejection 501s using an iterative constant fit ("fit"). (str; default: 501s 'dcr') 501s ovscsigma: If the deviation of mean overscan levels between a raw 501s input image and the reference image is higher than 501s |ovscsigma x stdev|, stop the processing. If 501s overscan="vpoly", this is used as sigma rejection level 501s for the iterative polynomial fit (the level comparison is 501s then done afterwards with |100 x stdev| to guard against 501s incompatible settings). Has no effect for 501s overscan="offset". (float; default: 30.0) 501s ovscignore: The number of pixels of the overscan adjacent to the data 501s section of the CCD that are ignored when computing 501s statistics or fits. (int; default: 3) 501s combine: Type of combination to use (str; default: 'sigclip') 501s nlow: Number of minimum pixels to reject with minmax (int; 501s default: 1) 501s nhigh: Number of maximum pixels to reject with minmax (int; 501s default: 1) 501s nkeep: Number of pixels to keep with minmax (int; default: 1) 501s lsigma: Low sigma for pixel rejection with sigclip (float; 501s default: 3.0) 501s hsigma: High sigma for pixel rejection with sigclip (float; 501s default: 3.0) 501s fbeam: Factor to describe the widening of the beam from the 501s focal plane to photo diode 2. (float; default: 1.1) 501s temp: Lamp temperature [K] used to create the black body 501s function. (float; default: 3200.0) 501s savemaster: Save the processed and combined master image before any 501s concolution is done. (bool; default: False) 501s savetable: Save the table with all the processed pixel values. 501s (bool; default: False) 501s merge: Merge output products from different IFUs into a common 501s file. (bool; default: False) 501s 501s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'BADPIX_TABLE', 501s 'GEOMETRY_TABLE', 'FILTER_LIST', 'TRACE_TABLE', 501s 'WAVECAL_TABLE'] 501s 501s Raw and product frames: 501s AMPL --> ['MASTER_AMPL', 'TABLE_AMPL', 'AMPL_CONVOLVED'] 501s Author: Peter Weilbacher 501s 501s 501s Recipe muse_astrometry: 501s version 2.8.7 501s 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'} 501s Docstring: Compute an astrometric solution. 501s 501s Merge pixel tables from all IFUs, apply correction for differential 501s atmospheric refraction (when necessary), optionally apply flux 501s calibration and telluric correction (if the necessary input data was 501s given), and resample the data from all exposures into a datacube. Use 501s the cube to detect objects which are then matched to their reference 501s positions from which a two-dimensional WCS solution is computed. There 501s are two pattern matching algorithm implemented, which can be selected 501s by chosing a positive or zero value of faccuracy. In the first method 501s (with a positive value of faccuracy), start using the search radius, 501s and iteratively decrease it, until no duplicate detections are 501s identified any more. Similarly, iterate the data accuracy (decrease it 501s downwards from the mean positioning error) until matches are found. 501s Remove the remaining unidentified objects. The second method (when 501s faccuracy is set to zero), iterates through all quadruples in both the 501s detected objects and the catalogue, calculates the transformation and 501s checks whether more than 80% of the detections match a catalog entry 501s within the radius. The main output is the ASTROMETRY_WCS file which is 501s a bare FITS header containing the world coordinate solution. The 501s secondary product is DATACUBE_ASTROMETRY, it is not needed for further 501s processing but can be used for verification and debugging. It contains 501s the reconstructed cube and two images created from it in further FITS 501s extensions: a white-light image and the special image created from the 501s central planes of the cube used to detect and centroid the stars (as 501s well as its variance). 501s 501s Parameters: 501s centroid: Centroiding method to use for objects in the field of 501s view. "gaussian" and "moffat" use 2D fits to derive the 501s centroid, "box" is a simple centroid in a square box. 501s (str; default: 'moffat') 501s detsigma: Source detection sigma level to use. If this is negative, 501s values between its absolute and 1.0 are tested with a 501s stepsize of 0.1, to find an optimal solution. (float; 501s default: 1.5) 501s radius: Initial radius in pixels for pattern matching 501s identification in the astrometric field. (float; default: 501s 3.0) 501s faccuracy: Factor of initial accuracy relative to mean positional 501s accuracy of the measured positions to use for pattern 501s matching. If this is set to zero, use the quadruples based 501s method. (float; default: 0.0) 501s niter: Number of iterations of the astrometric fit. (int; 501s default: 2) 501s rejsigma: Rejection sigma level of the astrometric fit. (float; 501s default: 3.0) 501s rotcenter: Center of rotation of the instrument, given as two comma- 501s separated floating point values in pixels. (str; default: 501s '-0.01,-1.20') 501s lambdamin: Cut off the data below this wavelength after loading the 501s pixel table(s). (float; default: 4000.0) 501s lambdamax: Cut off the data above this wavelength after loading the 501s pixel table(s). (float; default: 10000.0) 501s lambdaref: Reference wavelength used for correction of differential 501s atmospheric refraction. The R-band (peak wavelength ~7000 501s Angstrom) that is usually used for guiding, is close to 501s the central wavelength of MUSE, so a value of 7000.0 501s Angstrom should be used if nothing else is known. A value 501s less than zero switches DAR correction off. (float; 501s default: 7000.0) 501s darcheck: Carry out a check of the theoretical DAR correction using 501s source centroiding. If "correct" it will also apply an 501s empirical correction. (str; default: 'none') 501s 501s Calibration frames: ['ASTROMETRY_REFERENCE', 'EXTINCT_TABLE', 501s 'STD_RESPONSE', 'STD_TELLURIC'] 501s 501s Raw and product frames: 501s PIXTABLE_ASTROMETRY --> ['DATACUBE_ASTROMETRY', 'ASTROMETRY_WCS'] 501s Author: Peter Weilbacher 501s 501s 501s Recipe muse_scipost_subtract_sky: 501s version 2.8.7 501s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'orig': '', 'flux_sky': 0.0, 'flux_lamp': 0.0} 501s Docstring: Subtract night sky model. 501s 501s Subtract the sky as defined by the sky lines and continuum from a 501s pixel table. This is a separated task of muse_scipost. 501s 501s Parameters: 501s lambdamin: Cut off the data below this wavelength after loading the 501s pixel table(s). (float; default: 4000.0) 501s lambdamax: Cut off the data above this wavelength after loading the 501s pixel table(s). (float; default: 10000.0) 501s orig: If specified, write an additional column containing the 501s original data to the pixel table. (str; default: '') 501s flux_sky: Reference flat field flux, obtained by sky exposure. This 501s parameter is needed to scale the data of each pixel table 501s if more than one pixel table was used to determine the 501s sky. By default, it is taken from the parameter ESO DRS 501s MUSE FLAT FLUX SKY of the first pixel table. (float; 501s default: 0.0) 501s flux_lamp: Reference flat field flux, obtained by lamp exposure. This 501s parameter is needed to scale the data of each pixel table 501s if more than one pixel table was used to determine the 501s sky. By default, it is taken from the parameter ESO DRS 501s MUSE FLAT FLUX LAMP of the first pixel table. (float; 501s default: 0.0) 501s 501s Calibration frames: ['SKY_LINES', 'SKY_CONTINUUM', 'LSF_PROFILE'] 501s 501s Raw and product frames: 501s PIXTABLE_REDUCED --> ['PIXTABLE_REDUCED'] 501s Author: Ole Streicher 501s 501s 501s Recipe muse_geometry: 501s version 2.8.7 501s Parameters: {'ifu1': 1, 'ifu2': 24, 'sigma': 2.2, 'centroid': 'gaussian', 'smooth': 1.5, 'lambdamin': 6800.0, 'lambdamax': 7200.0} 501s Docstring: Compute relative location of the slices within the field of view and 501s measure the instrumental PSF on the detectors. 501s 501s Processing first works separately on each IFU of the raw input data 501s (in parallel): it trims the raw data and records the overscan 501s statistics, subtracts the bias and converts them from adu to count. 501s Optionally, the dark can be subtracted and the data can be divided by 501s the flat-field. The data of all input mask exposures is then averaged. 501s The averaged image together with the trace table and wavelength 501s calibration as well as the line catalog are used to detect spots. The 501s detection windows are used to measure the spots on all images of the 501s sequence, the result is saved, with information on the measured PSF, 501s in the spots tables. Then properties of all slices are computed, first 501s separately on each IFU to determine the peak position of the mask for 501s each slice and its angle, subsequently the width and horizontal 501s position. Then, the result of all IFUs is analyzed together to produce 501s a refined horizontal position, applying global shifts to each IFU as 501s needed. The vertical position is then determined using the known slice 501s ordering on the sky; the relative peak positions are put into 501s sequence, taking into account the vertical offsets of the pinholes in 501s the mask. The table is then cleaned up from intermediate debug data. 501s If the --smooth parameter is set to a positive value, it is used to do 501s a sigma-clipped smoothing within each slicer stack, for a more regular 501s appearance of the output table. The table is then saved. As a last 501s optional step, additional raw input data is reduced using the newly 501s geometry to produce an image of the field of view. If these exposures 501s contain smooth features, they can be used as a visual check of the 501s quality of the geometrical calibration. 501s 501s Parameters: 501s ifu1: First IFU to analyze. (int; default: 1) 501s ifu2: Last IFU to analyze. (int; default: 24) 501s sigma: Sigma detection level for spot detection, in terms of 501s median deviation above the median. (float; default: 2.2) 501s centroid: Type of centroiding and FWHM determination to use for all 501s spot measurements: simple barycenter method or using a 501s Gaussian fit. (str; default: 'gaussian') 501s smooth: Use this sigma-level cut for smoothing of the output table 501s within each slicer stack. Set to non-positive value to 501s deactivate smoothing. (float; default: 1.5) 501s lambdamin: When passing any MASK_CHECK frames in the input, use this 501s lower wavelength cut before reconstructing the image. 501s (float; default: 6800.0) 501s lambdamax: When passing any MASK_CHECK frames in the input, use this 501s upper wavelength cut before reconstructing the image. 501s (float; default: 7200.0) 501s 501s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 501s 'TRACE_TABLE', 'WAVECAL_TABLE', 'LINE_CATALOG', 501s 'BADPIX_TABLE', 'MASK_CHECK'] 501s 501s Raw and product frames: 501s MASK --> ['MASK_REDUCED', 'MASK_COMBINED', 'SPOTS_TABLE', 501s 'GEOMETRY_UNSMOOTHED', 'GEOMETRY_TABLE', 'GEOMETRY_CUBE'] 501s Author: Peter Weilbacher 501s 501s 501s Recipe muse_illum: 501s version 2.8.7 501s Parameters: {} 501s Docstring: Dummy recipe to convert a raw illumination flat field into a DFS 501s product 501s 501s The recipe copies the data of an illumination flat-field unmodified to 501s the output file. However it alters the header data such that the 501s result is a DFS compliant product file, which can be used in the on- 501s line pipeline environment to correct the illumination of twilight 501s and/or science observations. This recipe has no use in any environment 501s other than the on-line pipeline environment! 501s 501s No parameters 501s Calibration frames: [] 501s 501s Raw and product frames: 501s ILLUMFLAT --> ['ILLUM'] 501s Author: Ralf Palsa 501s 501s 501s Recipe muse_scipost_combine_pixtables: 501s version 2.8.7 501s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'weight': 'exptime'} 501s Docstring: Combine MUSE pixel tables, either from different IFUs, or from 501s different exposures, or both. 501s 501s Sort pixel tables by exposure and combine them with applied weights 501s into one big pixel table. This is a task separated from muse_scipost. 501s 501s Parameters: 501s lambdamin: Cut off the data below this wavelength after loading the 501s pixel table(s). (float; default: 4000.0) 501s lambdamax: Cut off the data above this wavelength after loading the 501s pixel table(s). (float; default: 10000.0) 501s weight: Type of weighting scheme to use when combining multiple 501s exposures. "exptime" just uses the exposure time to weight 501s the exposures, "fwhm" uses the DIMM information in the 501s header as well, "none" preserves an existing weight column 501s in the input pixel tables without changes. (str; default: 501s 'exptime') 501s 501s Calibration frames: ['OFFSET_LIST'] 501s 501s Raw and product frames: 501s PIXTABLE_OBJECT --> ['PIXTABLE_COMBINED'] 501s Author: Ole Streicher 501s 501s 501s Recipe muse_standard: 501s version 2.8.7 501s Parameters: {'profile': 'auto', 'select': 'distance', 'smooth': 'ppoly', 'lambdamin': 4000.0, 'lambdamax': 10000.0, 'lambdaref': 7000.0, 'darcheck': 'none', 'filter': 'white'} 501s Docstring: Create a flux response curve from a standard star exposure. 501s 501s Merge pixel tables from all IFUs and correct for differential 501s atmospheric refraction, when necessary. To derive the flux response 501s curve, integrate the flux of all objects detected within the field of 501s view using the given profile. Select one object as the standard star 501s (either the brightest or the one nearest one, depending on --select) 501s and compare its measured fluxes to tabulated fluxes to derive the 501s sensitivity over wavelength. Postprocess this sensitivity curve to 501s mark wavelength ranges affected by telluric absorption. Interpolate 501s over the telluric regions and derive a telluric correction spectrum 501s for them. The final response curve is then linearly extrapolated to 501s the largest possible MUSE wavelength range and smoothed (with the 501s method given by --smooth). The derivation of the telluric correction 501s spectrum assumes that the star has a smooth spectrum within the 501s telluric regions. If there are more than one exposure given in the 501s input data, the derivation of the flux response and telluric 501s corrections are done separately for each exposure. For each exposure, 501s an image containing the extracted stellar spectra and the datacube 501s used for flux integration are saved, together with collapsed images 501s for each given filter. In MUSE's WFM data (both AO and non-AO), the 501s Moffat profile is a good approximation of the actual PSF. Using the 501s smoothed profile ("smoffat") helps to increase the S/N and in most 501s cases removes systematics. In NFM, however, the profile is a 501s combination of a wide PSF plus the central AO-corrected peak, which 501s cannot be fit well by an analytical profile. In this case the circular 501s aperture is the best way to extract the flux. Using --profile="auto" 501s (the default) selects these options to give the best flux extraction 501s for most cases. 501s 501s Parameters: 501s profile: Type of flux integration to use. "gaussian", "moffat", and 501s "smoffat" use 2D profile fitting, "circle" and "square" 501s are non-optimal aperture flux integrators. "smoffat" uses 501s smoothing of the Moffat parameters from an initial fit, to 501s derive physically meaningful wavelength- dependent 501s behavior. "auto" selects the smoothed Moffat profile for 501s WFM data and circular flux integration for NFM. (str; 501s default: 'auto') 501s select: How to select the star for flux integration, "flux" uses 501s the brightest star in the field, "distance" uses the 501s detection nearest to the approximate coordinates of the 501s reference source. (str; default: 'distance') 501s smooth: How to smooth the response curve before writing it to 501s disk. "none" does not do any kind of smoothing (such a 501s response curve is only useful, if smoothed externally; 501s "median" does a median-filter of 15 Angstrom half-width; 501s "ppoly" fits piecewise cubic polynomials (each one across 501s 2x150 Angstrom width) postprocessed by a sliding average 501s filter of 15 Angstrom half-width. (str; default: 'ppoly') 501s lambdamin: Cut off the data below this wavelength after loading the 501s pixel table(s). (float; default: 4000.0) 501s lambdamax: Cut off the data above this wavelength after loading the 501s pixel table(s). (float; default: 10000.0) 501s lambdaref: Reference wavelength used for correction of differential 501s atmospheric refraction. The R-band (peak wavelength ~7000 501s Angstrom) that is usually used for guiding, is close to 501s the central wavelength of MUSE, so a value of 7000.0 501s Angstrom should be used if nothing else is known. A value 501s less than zero switches DAR correction off. (float; 501s default: 7000.0) 501s darcheck: Carry out a check of the theoretical DAR correction using 501s source centroiding. If "correct" it will also apply an 501s empirical correction. (str; default: 'none') 501s filter: The filter name(s) to be used for the output field-of-view 501s image. Each name has to correspond to an EXTNAME in an 501s extension of the FILTER_LIST file. If an unsupported 501s filter name is given, creation of the respective image is 501s omitted. If multiple filter names are given, they have to 501s be comma separated. If the zeropoint QC parameters are 501s wanted, make sure to add "Johnson_V,Cousins_R,Cousins_I". 501s (str; default: 'white') 501s 501s Calibration frames: ['EXTINCT_TABLE', 'STD_FLUX_TABLE', 501s 'TELLURIC_REGIONS', 'FILTER_LIST'] 501s 501s Raw and product frames: 501s PIXTABLE_STD --> ['DATACUBE_STD', 'STD_FLUXES', 'STD_RESPONSE', 501s 'STD_TELLURIC'] 501s Author: Peter Weilbacher 501s 501s 501s Recipe muse_create_sky: 501s version 2.8.7 501s 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} 501s Docstring: Create night sky model from selected pixels of an exposure of empty 501s sky. 501s 501s This recipe creates the continuum and the atmospheric transition line 501s spectra of the night sky from the data in a pixel table(s) belonging 501s to one exposure of (mostly) empty sky. 501s 501s Parameters: 501s fraction: Fraction of the image (without the ignored part) to be 501s considered as sky. If an input sky mask is provided, the 501s fraction is applied to the regions within the mask. If the 501s whole sky mask should be used, set this parameter to 1. 501s (float; default: 0.75) 501s ignore: Fraction of the image to be ignored. If an input sky mask 501s is provided, the fraction is applied to the regions within 501s the mask. If the whole sky mask should be used, set this 501s parameter to 0. (float; default: 0.05) 501s sampling: Spectral sampling of the sky spectrum [Angstrom]. (float; 501s default: 0.3125) 501s csampling: Spectral sampling of the continuum spectrum [Angstrom]. 501s (float; default: 0.3125) 501s crsigma: Sigma level clipping for cube-based and spectrum-based CR 501s rejection. This has to be a string of two comma-separated 501s floating-point numbers. The first value gives the sigma- 501s level rejection for cube-based CR rejection (using 501s "median", see muse_scipost), the second value the sigma- 501s level for spectrum-based CR cleaning. Both can be switched 501s off, by passing zero or a negative value. (str; default: 501s '15.,15.') 501s lambdamin: Cut off the data below this wavelength after loading the 501s pixel table(s). (float; default: 4000.0) 501s lambdamax: Cut off the data above this wavelength after loading the 501s pixel table(s). (float; default: 10000.0) 501s lambdaref: Reference wavelength used for correction of differential 501s atmospheric refraction. The R-band (peak wavelength ~7000 501s Angstrom) that is usually used for guiding, is close to 501s the central wavelength of MUSE, so a value of 7000.0 501s Angstrom should be used if nothing else is known. A value 501s less than zero switches DAR correction off. (float; 501s default: 7000.0) 501s 501s Calibration frames: ['EXTINCT_TABLE', 'STD_RESPONSE', 'STD_TELLURIC', 501s 'SKY_LINES', 'SKY_CONTINUUM', 'LSF_PROFILE', 501s 'SKY_MASK'] 501s 501s Raw and product frames: 501s PIXTABLE_SKY --> ['SKY_MASK', 'SKY_IMAGE', 'SKY_SPECTRUM', 501s 'SKY_LINES', 'SKY_CONTINUUM'] 501s Author: Ole Streicher 501s 501s 501s Recipe muse_exp_combine: 501s version 2.8.7 501s 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} 502s Docstring: Combine several exposures into one datacube. 502s 502s Sort reduced pixel tables, one per exposure, by exposure and combine 502s them with applied weights into one final datacube. 502s 502s Parameters: 502s save: Select output product(s) to save. Can contain one or more 502s of "cube" (output cube and associated images; if this is 502s not given, no resampling is done at all) or "combined" 502s (fully reduced and combined pixel table for the full set 502s of exposures; this is useful, if the final resampling step 502s is to be done again separately). If several options are 502s given, they have to be comma-separated. (str; default: 502s 'cube') 502s resample: The resampling technique to use for the final output cube. 502s (str; default: 'drizzle') 502s dx: Horizontal step size for resampling (in arcsec or pixel). 502s The following defaults are taken when this value is set to 502s 0.0: 0.2'' for WFM, 0.025'' for NFM, 1.0 if data is in 502s pixel units. (float; default: 0.0) 502s dy: Vertical step size for resampling (in arcsec or pixel). 502s The following defaults are taken when this value is set to 502s 0.0: 0.2'' for WFM, 0.025'' for NFM, 1.0 if data is in 502s pixel units. (float; default: 0.0) 502s dlambda: Wavelength step size (in Angstrom). Natural instrument 502s sampling is used, if this is 0.0 (float; default: 0.0) 502s crtype: Type of statistics used for detection of cosmic rays 502s during final resampling. "iraf" uses the variance 502s information, "mean" uses standard (mean/stdev) statistics, 502s "median" uses median and the median median of the absolute 502s median deviation. (str; default: 'median') 502s crsigma: Sigma rejection factor to use for cosmic ray rejection 502s during final resampling. A zero or negative value switches 502s cosmic ray rejection off. (float; default: 10.0) 502s rc: Critical radius for the "renka" resampling method. (float; 502s default: 1.25) 502s pixfrac: Pixel down-scaling factor for the "drizzle" resampling 502s method. Up to three, comma-separated, floating-point 502s values can be given. If only one value is given, it 502s applies to all dimensions, two values are interpreted as 502s spatial and spectral direction, respectively, while three 502s are taken as horizontal, vertical, and spectral. (str; 502s default: '0.6,0.6') 502s ld: Number of adjacent pixels to take into account during 502s resampling in all three directions (loop distance); this 502s affects all resampling methods except "nearest". (int; 502s default: 1) 502s format: Type of output file format, "Cube" is a standard FITS cube 502s with NAXIS=3 and multiple extensions (for data and 502s variance). The extended "x" formats include the 502s reconstructed image(s) in FITS image extensions within the 502s same file. "sdpCube" does some extra calculations to 502s create FITS keywords for the ESO Science Data Products. 502s (str; default: 'Cube') 502s weight: Type of weighting scheme to use when combining multiple 502s exposures. "exptime" just uses the exposure time to weight 502s the exposures, "fwhm" uses the best available seeing 502s information from the headers as well, "header" queries 502s ESO.DRS.MUSE.WEIGHT of each input file instead of the 502s FWHM, and "none" preserves an existing weight column in 502s the input pixel tables without changes. (str; default: 502s 'exptime') 502s filter: The filter name(s) to be used for the output field-of-view 502s image. Each name has to correspond to an EXTNAME in an 502s extension of the FILTER_LIST file. If an unsupported 502s filter name is given, creation of the respective image is 502s omitted. If multiple filter names are given, they have to 502s be comma separated. (str; default: 'white') 502s lambdamin: Cut off the data below this wavelength after loading the 502s pixel table(s). (float; default: 4000.0) 502s lambdamax: Cut off the data above this wavelength after loading the 502s pixel table(s). (float; default: 10000.0) 502s 502s Calibration frames: ['OFFSET_LIST', 'FILTER_LIST', 'OUTPUT_WCS'] 502s 502s Raw and product frames: 502s PIXTABLE_REDUCED --> ['DATACUBE_FINAL', 'IMAGE_FOV', 502s 'PIXTABLE_COMBINED'] 502s Author: Peter Weilbacher 502s 502s 502s Recipe muse_scipost_raman: 502s version 2.8.7 502s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'lambdaref': 7000.0, 'width': 20.0, 'crsigma': 15.0, 'fraction': 0.75, 'ignore': 0.05} 502s Docstring: Remove of 4GLSF Raman emission. 502s 502s This recipe removes the Raman scattered light of the 4GLSF system from 502s the exposure. It must be before the normal sky subtraction. 502s 502s Parameters: 502s lambdamin: Cut off the data below this wavelength after loading the 502s pixel table(s). (float; default: 4000.0) 502s lambdamax: Cut off the data above this wavelength after loading the 502s pixel table(s). (float; default: 10000.0) 502s lambdaref: Reference wavelength used for correction of differential 502s atmospheric refraction. The R-band (peak wavelength ~7000 502s Angstrom) that is usually used for guiding, is close to 502s the central wavelength of MUSE, so a value of 7000.0 502s Angstrom should be used if nothing else is known. A value 502s less than zero switches DAR correction off. (float; 502s default: 7000.0) 502s width: Wavelength range around Raman lines [Angstrom]. (float; 502s default: 20.0) 502s crsigma: Sigma level clipping for cube-based CR rejection (using 502s "median", see muse_scipost). It can be switched off, by 502s passing zero or a negative value. (float; default: 15.0) 502s fraction: Fraction of the image (without the ignored part) to be 502s considered as sky. If an input sky mask is provided, the 502s fraction is applied to the regions within the mask. If the 502s whole sky mask should be used, set this parameter to 1. 502s (float; default: 0.75) 502s ignore: Lowest fraction of the image to be ignored. If an input 502s sky mask is provided, the fraction is applied to the 502s regions within the mask. If the whole sky mask should be 502s used, set this parameter to 0. (float; default: 0.05) 502s 502s Calibration frames: ['RAMAN_LINES', 'LSF_PROFILE', 'SKY_MASK'] 502s 502s Raw and product frames: 502s PIXTABLE_OBJECT --> ['RAMAN_IMAGES', 'PIXTABLE_REDUCED'] 502s Author: Ole Streicher 502s 502s 502s Recipe muse_lsf: 502s version 2.8.7 502s 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'} 502s Docstring: Compute the LSF 502s 502s Compute the slice and wavelength dependent LSF from a lines spectrum 502s (ARC lamp). 502s 502s Parameters: 502s nifu: IFU to handle. If set to 0, all IFUs are 502s processed serially. If set to -1, all IFUs are 502s processed in parallel. (int; default: 0) 502s overscan: If this is "none", stop when detecting 502s discrepant overscan levels (see ovscsigma), 502s for "offset" it assumes that the mean overscan 502s level represents the real offset in the bias 502s levels of the exposures involved, and adjusts 502s the data accordingly; for "vpoly", a 502s polynomial is fit to the vertical overscan and 502s subtracted from the whole quadrant. (str; 502s default: 'vpoly') 502s ovscreject: This influences how values are rejected when 502s computing overscan statistics. Either no 502s rejection at all ("none"), rejection using the 502s DCR algorithm ("dcr"), or rejection using an 502s iterative constant fit ("fit"). (str; default: 502s 'dcr') 502s ovscsigma: If the deviation of mean overscan levels 502s between a raw input image and the reference 502s image is higher than |ovscsigma x stdev|, stop 502s the processing. If overscan="vpoly", this is 502s used as sigma rejection level for the 502s iterative polynomial fit (the level comparison 502s is then done afterwards with |100 x stdev| to 502s guard against incompatible settings). Has no 502s effect for overscan="offset". (float; default: 502s 30.0) 502s ovscignore: The number of pixels of the overscan adjacent 502s to the data section of the CCD that are 502s ignored when computing statistics or fits. 502s (int; default: 3) 502s save_subtracted: Save the pixel table after the LSF 502s subtraction. (bool; default: False) 502s line_quality: Minimal quality flag in line catalog for 502s selection (int; default: 3) 502s lsf_range: Wavelength window (half size) around each line 502s to estimate LSF (float; default: 7.5) 502s lsf_size: Image size in LSF direction (int; default: 502s 150) 502s lambda_size: Image size in line wavelength direction (int; 502s default: 30) 502s lsf_regression_window: Size of the regression window in LSF direction 502s (float; default: 0.7) 502s merge: Merge output products from different IFUs into 502s a common file. (bool; default: False) 502s combine: Type of lampwise image combination to use. 502s (str; default: 'sigclip') 502s method: LSF generation method. Depending on this 502s value, either an interpolated LSF cube is 502s created, or a table with the parameters of a 502s hermitean gaussian. (str; default: 502s 'interpolate') 502s 502s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 502s 'TRACE_TABLE', 'WAVECAL_TABLE', 'BADPIX_TABLE', 502s 'LINE_CATALOG'] 502s 502s Raw and product frames: 502s ARC --> ['LSF_PROFILE', 'PIXTABLE_SUBTRACTED'] 502s ARC_LSF --> ['LSF_PROFILE', 'PIXTABLE_SUBTRACTED'] 502s Author: Ole Streicher 502s 502s 502s Recipe muse_scipost_make_cube: 502s version 2.8.7 502s 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'} 502s Docstring: Make a MUSE cube from a MUSE pixel table. 502s 502s This recipe takes a pixel table and resamples it to either a FITS cube 502s or a Euro3D table and optionally to a stacked spectrum. This is a part 502s of the muse_scipost recipe. 502s 502s Parameters: 502s lambdamin: Cut off the data below this wavelength after loading the 502s pixel table(s). (float; default: 4000.0) 502s lambdamax: Cut off the data above this wavelength after loading the 502s pixel table(s). (float; default: 10000.0) 502s resample: The resampling technique to use for the final output cube. 502s (str; default: 'drizzle') 502s dx: Horizontal step size for resampling (in arcsec or pixel). 502s The following defaults are taken when this value is set to 502s 0.0: 0.2'' for WFM, 0.025'' for NFM, 1.0 if data is in 502s pixel units. (float; default: 0.0) 502s dy: Vertical step size for resampling (in arcsec or pixel). 502s The following defaults are taken when this value is set to 502s 0.0: 0.2'' for WFM, 0.025'' for NFM, 1.0 if data is in 502s pixel units. (float; default: 0.0) 502s dlambda: Wavelength step size (in Angstrom). Natural instrument 502s sampling is used, if this is 0.0 (float; default: 0.0) 502s crtype: Type of statistics used for detection of cosmic rays 502s during final resampling. "iraf" uses the variance 502s information, "mean" uses standard (mean/stdev) statistics, 502s "median" uses median and the median median of the absolute 502s median deviation. (str; default: 'median') 502s crsigma: Sigma rejection factor to use for cosmic ray rejection 502s during final resampling. A zero or negative value switches 502s cosmic ray rejection off. (float; default: 15.0) 502s rc: Critical radius for the "renka" resampling method. (float; 502s default: 1.25) 502s pixfrac: Pixel down-scaling factor for the "drizzle" resampling 502s method. Up to three, comma-separated, floating-point 502s values can be given. If only one value is given, it 502s applies to all dimensions, two values are interpreted as 502s spatial and spectral direction, respectively, while three 502s are taken as horizontal, vertical, and spectral. (str; 502s default: '0.8,0.8') 502s ld: Number of adjacent pixels to take into account during 502s resampling in all three directions (loop distance); this 502s affects all resampling methods except "nearest". (int; 502s default: 1) 502s format: Type of output file format, "Cube" is a standard FITS cube 502s with NAXIS=3 and multiple extensions (for data and 502s variance). The extended "x" formats include the 502s reconstructed image(s) in FITS image extensions within the 502s same file. (str; default: 'Cube') 502s stacked: If true, write an additional output file in form of a 2D 502s stacked image (x direction is pseudo-spatial, y direction 502s is wavelength). (bool; default: False) 502s filter: The filter name(s) to be used for the output field-of-view 502s image. Each name has to correspond to an EXTNAME in an 502s extension of the FILTER_LIST file. If an unsupported 502s filter name is given, creation of the respective image is 502s omitted. If multiple filter names are given, they have to 502s be comma separated. (str; default: 'white') 502s 502s Calibration frames: ['FILTER_LIST', 'OUTPUT_WCS'] 502s 502s Raw and product frames: 502s PIXTABLE_OBJECT --> ['DATACUBE_FINAL', 'IMAGE_FOV', 502s 'OBJECT_RESAMPLED'] 502s Author: Ole Streicher 502s 502s 502s Recipe muse_scibasic: 502s version 2.8.7 502s 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} 502s Docstring: Remove the instrumental signature from the data of each CCD and 502s convert them from an image into a pixel table. 502s 502s Processing handles each raw input image separately: it trims the raw 502s data and records the overscan statistics, subtracts the bias (taking 502s account of the overscan, if --overscan is not "none"), optionally 502s detects cosmic rays (note that by default cosmic ray rejection is 502s handled in the post processing recipes while the data is reformatted 502s into a datacube, so that the default setting is cr="none" here), 502s converts the images from adu to count, subtracts the dark, divides by 502s the flat-field, and (optionally) propagates the integrated flux value 502s from the twilight-sky cube. The reduced image is then saved (if 502s --saveimage=true). The input calibrations geometry table, trace table, 502s and wavelength calibration table are used to assign 3D coordinates to 502s each CCD-based pixel, thereby creating a pixel table for each 502s exposure. If --skylines contains one or more wavelengths for (bright 502s and isolated) sky emission lines, these lines are used to correct the 502s wavelength calibration using an offset. The data is then cut to a 502s useful wavelength range (if --crop=true). If an ILLUM exposure was 502s given as input, it is then used to correct the relative illumination 502s between all slices of one IFU. For this, the data of each slice is 502s multiplied by the normalized median flux of that slice in the ILLUM 502s exposure. As last step, the data is divided by the normalized twilight 502s cube (if given), using the 3D coordinate of each pixel in the pixel 502s table to interpolate the twilight correction onto the data. This pre- 502s reduced pixel table for each exposure is then saved to disk. 502s 502s Parameters: 502s nifu: IFU to handle. If set to 0, all IFUs are processed 502s serially. If set to -1, all IFUs are processed in 502s parallel. (int; default: 0) 502s overscan: If this is "none", stop when detecting discrepant 502s overscan levels (see ovscsigma), for "offset" it 502s assumes that the mean overscan level represents the 502s real offset in the bias levels of the exposures 502s involved, and adjusts the data accordingly; for 502s "vpoly", a polynomial is fit to the vertical overscan 502s and subtracted from the whole quadrant. (str; default: 502s 'vpoly') 502s ovscreject: This influences how values are rejected when computing 502s overscan statistics. Either no rejection at all 502s ("none"), rejection using the DCR algorithm ("dcr"), or 502s rejection using an iterative constant fit ("fit"). 502s (str; default: 'dcr') 502s ovscsigma: If the deviation of mean overscan levels between a raw 502s input image and the reference image is higher than 502s |ovscsigma x stdev|, stop the processing. If 502s overscan="vpoly", this is used as sigma rejection level 502s for the iterative polynomial fit (the level comparison 502s is then done afterwards with |100 x stdev| to guard 502s against incompatible settings). Has no effect for 502s overscan="offset". (float; default: 30.0) 502s ovscignore: The number of pixels of the overscan adjacent to the 502s data section of the CCD that are ignored when computing 502s statistics or fits. (int; default: 3) 502s crop: Automatically crop the output pixel tables in 502s wavelength depending on the expected useful wavelength 502s range of the active instrument mode (4750-9350 Angstrom 502s for nominal mode and NFM, 4700-9350 Angstrom for 502s nominal AO mode, and 4600-9350 Angstrom for the 502s extended modes). (bool; default: True) 502s cr: Type of cosmic ray cleaning to use (for quick-look data 502s processing). (str; default: 'none') 502s xbox: Search box size in x. Only used if cr=dcr. (int; 502s default: 15) 502s ybox: Search box size in y. Only used if cr=dcr. (int; 502s default: 40) 502s passes: Maximum number of cleaning passes. Only used if cr=dcr. 502s (int; default: 2) 502s thres: Threshold for detection gap in factors of standard 502s deviation. Only used if cr=dcr. (float; default: 5.8) 502s combine: Type of combination to use. Note that in most cases, 502s science exposures cannot easily be combined on the CCD 502s level, so this should usually be kept as "none"! This 502s does not pay attention about the type of input data, 502s and will combine all raw inputs! (str; default: 'none') 502s nlow: Number of minimum pixels to reject with minmax (int; 502s default: 1) 502s nhigh: Number of maximum pixels to reject with minmax (int; 502s default: 1) 502s nkeep: Number of pixels to keep with minmax (int; default: 1) 502s lsigma: Low sigma for pixel rejection with sigclip (float; 502s default: 3.0) 502s hsigma: High sigma for pixel rejection with sigclip (float; 502s default: 3.0) 502s scale: Scale the individual images to a common exposure time 502s before combining them. (bool; default: True) 502s saveimage: Save the pre-processed CCD-based image of each input 502s exposure before it is transformed into a pixel table. 502s (bool; default: True) 502s skylines: List of wavelengths of sky emission lines (in Angstrom) 502s to use as reference for wavelength offset correction 502s using a Gaussian fit. It can contain multiple 502s (isolated) lines, as comma-separated list, individual 502s shifts are then combined into one weighted average 502s offset. Set to "none" to deactivate. (str; default: 502s '5577.339,6300.304') 502s skyhalfwidth: Half-width of the extraction box (in Angstrom) around 502s each sky emission line. (float; default: 5.0) 502s skybinsize: Size of the bins (in Angstrom per pixel) for the 502s intermediate spectrum to do the Gaussian fit to each 502s sky emission line. (float; default: 0.1) 502s skyreject: Sigma clipping parameters for the intermediate spectrum 502s to do the Gaussian fit to each sky emission line. Up to 502s three comma-separated numbers can be given, which are 502s interpreted as high sigma-clipping limit (float), low 502s limit (float), and number of iterations (integer), 502s respectively. (str; default: '15.,15.,1') 502s resample: Resample the input science data into 2D spectral images 502s using all supplied calibrations for a visual check. 502s Note that the image produced will show small wiggles 502s even when the input calibrations are good and were 502s applied successfully! (bool; default: False) 502s dlambda: Wavelength step (in Angstrom per pixel) to use for 502s resampling. (float; default: 1.25) 502s merge: Merge output products from different IFUs into a common 502s file. (bool; default: False) 502s 502s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 502s 'TRACE_TABLE', 'WAVECAL_TABLE', 'GEOMETRY_TABLE', 502s 'TWILIGHT_CUBE', 'BADPIX_TABLE'] 502s 502s Raw and product frames: 502s OBJECT --> ['OBJECT_RED', 'OBJECT_RESAMPLED', 'PIXTABLE_OBJECT'] 502s STD --> ['STD_RED', 'STD_RESAMPLED', 'PIXTABLE_STD'] 502s SKY --> ['SKY_RED', 'SKY_RESAMPLED', 'PIXTABLE_SKY'] 502s ASTROMETRY --> ['ASTROMETRY_RED', 'ASTROMETRY_RESAMPLED', 502s 'PIXTABLE_ASTROMETRY'] 502s ILLUM --> [] 502s REDUCED --> ['REDUCED_RESAMPLED', 'PIXTABLE_REDUCED'] 502s Author: Peter Weilbacher 502s 502s 502s autopkgtest [01:01:22]: test test-recipe.py: -----------------------] 503s autopkgtest [01:01:23]: test test-recipe.py: - - - - - - - - - - results - - - - - - - - - - 503s test-recipe.py PASS (superficial) 504s autopkgtest [01:01:24]: @@@@@@@@@@@@@@@@@@@@ summary 504s test-recipe.py PASS (superficial) 521s Creating nova instance adt-noble-arm64-cpl-plugin-muse-20240419-005300-juju-7f2275-prod-proposed-migration-environment-3-281f50e2-1df8-4754-8bde-6ae765045a5d from image adt/ubuntu-noble-arm64-server-20240418.img (UUID 6f8e97a7-9a55-4e99-9797-31213b709dd4)...