0s autopkgtest [23:45:17]: starting date and time: 2024-04-18 23:45:17+0000 0s autopkgtest [23:45:17]: git checkout: 43bc6cdf gitlab-ci: do not include the salsa pipeline 0s autopkgtest [23:45:17]: host juju-7f2275-prod-proposed-migration-environment-2; command line: /home/ubuntu/autopkgtest/runner/autopkgtest --output-dir /tmp/autopkgtest-work.nepmfbon/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-2@bos02-ppc64el-5.secgroup --name adt-noble-ppc64el-cpl-plugin-muse-20240418-234516-juju-7f2275-prod-proposed-migration-environment-2-469103a9-8abd-4ed9-8266-b58b69860d31 --image adt/ubuntu-noble-ppc64el-server --keyname testbed-juju-7f2275-prod-proposed-migration-environment-2 --net-id=net_prod-proposed-migration -e TERM=linux -e ''"'"'http_proxy=http://squid.internal:3128'"'"'' -e ''"'"'https_proxy=http://squid.internal:3128'"'"'' -e ''"'"'no_proxy=127.0.0.1,127.0.1.1,login.ubuntu.com,localhost,localdomain,novalocal,internal,archive.ubuntu.com,ports.ubuntu.com,security.ubuntu.com,ddebs.ubuntu.com,changelogs.ubuntu.com,launchpadlibrarian.net,launchpadcontent.net,launchpad.net,10.24.0.0/24,keystone.ps5.canonical.com,objectstorage.prodstack5.canonical.com'"'"'' --mirror=http://ftpmaster.internal/ubuntu/ 153s autopkgtest [23:47:50]: testbed dpkg architecture: ppc64el 153s autopkgtest [23:47:50]: testbed apt version: 2.7.14build2 153s autopkgtest [23:47:50]: @@@@@@@@@@@@@@@@@@@@ test bed setup 154s Get:1 http://ftpmaster.internal/ubuntu noble-proposed InRelease [117 kB] 155s Get:2 http://ftpmaster.internal/ubuntu noble-proposed/multiverse Sources [2340 B] 155s Get:3 http://ftpmaster.internal/ubuntu noble-proposed/universe Sources [381 kB] 155s Get:4 http://ftpmaster.internal/ubuntu noble-proposed/main Sources [57.5 kB] 155s Get:5 http://ftpmaster.internal/ubuntu noble-proposed/restricted Sources [12.2 kB] 155s Get:6 http://ftpmaster.internal/ubuntu noble-proposed/main ppc64el Packages [112 kB] 155s Get:7 http://ftpmaster.internal/ubuntu noble-proposed/main ppc64el c-n-f Metadata [3116 B] 155s Get:8 http://ftpmaster.internal/ubuntu noble-proposed/restricted ppc64el Packages [976 B] 155s Get:9 http://ftpmaster.internal/ubuntu noble-proposed/restricted ppc64el c-n-f Metadata [116 B] 155s Get:10 http://ftpmaster.internal/ubuntu noble-proposed/universe ppc64el Packages [587 kB] 155s Get:11 http://ftpmaster.internal/ubuntu noble-proposed/universe ppc64el c-n-f Metadata [8652 B] 155s Get:12 http://ftpmaster.internal/ubuntu noble-proposed/multiverse ppc64el Packages [1004 B] 155s Get:13 http://ftpmaster.internal/ubuntu noble-proposed/multiverse ppc64el c-n-f Metadata [116 B] 158s Fetched 1282 kB in 1s (1211 kB/s) 158s Reading package lists... 159s sh: 4: dhclient: not found 160s Reading package lists... 160s Building dependency tree... 160s Reading state information... 160s Calculating upgrade... 161s The following packages will be upgraded: 161s libkeyutils1 libnuma1 make netcat-openbsd numactl 161s 5 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 161s Need to get 343 kB of archives. 161s After this operation, 16.4 kB disk space will be freed. 161s Get:1 http://ftpmaster.internal/ubuntu noble/main ppc64el libkeyutils1 ppc64el 1.6.3-3build1 [11.0 kB] 161s Get:2 http://ftpmaster.internal/ubuntu noble/main ppc64el netcat-openbsd ppc64el 1.226-1ubuntu2 [46.2 kB] 161s Get:3 http://ftpmaster.internal/ubuntu noble/main ppc64el libnuma1 ppc64el 2.0.18-1build1 [28.2 kB] 161s Get:4 http://ftpmaster.internal/ubuntu noble/main ppc64el make ppc64el 4.3-4.1build2 [214 kB] 161s Get:5 http://ftpmaster.internal/ubuntu noble/main ppc64el numactl ppc64el 2.0.18-1build1 [43.9 kB] 161s Fetched 343 kB in 1s (633 kB/s) 162s (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 ... 71981 files and directories currently installed.) 162s Preparing to unpack .../libkeyutils1_1.6.3-3build1_ppc64el.deb ... 162s Unpacking libkeyutils1:ppc64el (1.6.3-3build1) over (1.6.3-3) ... 162s Preparing to unpack .../netcat-openbsd_1.226-1ubuntu2_ppc64el.deb ... 162s Unpacking netcat-openbsd (1.226-1ubuntu2) over (1.226-1ubuntu1) ... 162s Preparing to unpack .../libnuma1_2.0.18-1build1_ppc64el.deb ... 162s Unpacking libnuma1:ppc64el (2.0.18-1build1) over (2.0.18-1) ... 162s Preparing to unpack .../make_4.3-4.1build2_ppc64el.deb ... 162s Unpacking make (4.3-4.1build2) over (4.3-4.1build1) ... 162s Preparing to unpack .../numactl_2.0.18-1build1_ppc64el.deb ... 162s Unpacking numactl (2.0.18-1build1) over (2.0.18-1) ... 162s Setting up libkeyutils1:ppc64el (1.6.3-3build1) ... 162s Setting up netcat-openbsd (1.226-1ubuntu2) ... 162s Setting up make (4.3-4.1build2) ... 162s Setting up libnuma1:ppc64el (2.0.18-1build1) ... 162s Setting up numactl (2.0.18-1build1) ... 162s Processing triggers for man-db (2.12.0-4build1) ... 163s Processing triggers for libc-bin (2.39-0ubuntu8) ... 163s Reading package lists... 163s Building dependency tree... 163s Reading state information... 163s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 163s Hit:1 http://ftpmaster.internal/ubuntu noble-proposed InRelease 164s Hit:2 http://ftpmaster.internal/ubuntu noble InRelease 164s Hit:3 http://ftpmaster.internal/ubuntu noble-updates InRelease 164s Hit:4 http://ftpmaster.internal/ubuntu noble-security InRelease 165s Reading package lists... 165s Reading package lists... 165s Building dependency tree... 165s Reading state information... 165s Calculating upgrade... 165s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 165s Reading package lists... 166s Building dependency tree... 166s Reading state information... 166s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 169s autopkgtest [23:48:06]: testbed running kernel: Linux 6.8.0-22-generic #22-Ubuntu SMP Thu Apr 4 22:47:57 UTC 2024 169s autopkgtest [23:48:06]: @@@@@@@@@@@@@@@@@@@@ apt-source cpl-plugin-muse 172s Get:1 http://ftpmaster.internal/ubuntu noble/universe cpl-plugin-muse 2.8.7+dfsg-3 (dsc) [2420 B] 172s Get:2 http://ftpmaster.internal/ubuntu noble/universe cpl-plugin-muse 2.8.7+dfsg-3 (tar) [1586 kB] 172s Get:3 http://ftpmaster.internal/ubuntu noble/universe cpl-plugin-muse 2.8.7+dfsg-3 (diff) [14.6 kB] 172s gpgv: Signature made Tue Aug 16 06:12:08 2022 UTC 172s gpgv: using RSA key BAFC6C85F7CB143FEEB6FB157115AFD07710DCF7 172s gpgv: Can't check signature: No public key 172s dpkg-source: warning: cannot verify inline signature for ./cpl-plugin-muse_2.8.7+dfsg-3.dsc: no acceptable signature found 172s autopkgtest [23:48:09]: testing package cpl-plugin-muse version 2.8.7+dfsg-3 173s autopkgtest [23:48:10]: build not needed 179s autopkgtest [23:48:16]: test test-recipe.py: preparing testbed 180s Reading package lists... 180s Building dependency tree... 180s Reading state information... 180s Starting pkgProblemResolver with broken count: 0 180s Starting 2 pkgProblemResolver with broken count: 0 180s Done 180s The following additional packages will be installed: 180s cpl-plugin-muse libblas3 libcext0 libcfitsio10t64 libcplcore26 libcpldfs26 180s libcpldrs26 libcplui26 liberfa1 libfftw3-double3 libfftw3-single3 180s libgfortran5 libgomp1 libgsl27 libgslcblas0 libjs-jquery 180s libjs-jquery-hotkeys libjs-jquery-isonscreen libjs-jquery-metadata 180s libjs-jquery-tablesorter libjs-jquery-throttle-debounce libjs-sphinxdoc 180s libjs-underscore liblapack3 libwcs8 python3-astropy 180s python3-astropy-iers-data python3-coverage python3-cpl python3-dateutil 180s python3-erfa python3-hypothesis python3-iniconfig python3-numpy 180s python3-packaging python3-pluggy python3-ply python3-pytest 180s python3-pytest-arraydiff python3-pytest-astropy 180s python3-pytest-astropy-header python3-pytest-cov python3-pytest-doctestplus 180s python3-pytest-filter-subpackage python3-pytest-mock 180s python3-pytest-remotedata python3-sortedcontainers 180s Suggested packages: 180s cpl-plugin-muse-calib cpl-plugin-muse-doc libfftw3-bin libfftw3-dev 180s gsl-ref-psdoc | gsl-doc-pdf | gsl-doc-info | gsl-ref-html libxml2-utils 180s python-astropy-doc python3-astropy-affiliated python3-bs4 python3-h5py 180s python3-matplotlib python3-pandas python-coverage-doc gdb 180s python-hypothesis-doc gcc gfortran python3-dev python-ply-doc 180s python-pytest-mock-doc python-sortedcontainers-doc 180s Recommended packages: 180s javascript-common libjs-jquery-datatables python3-scipy python3-click 180s The following NEW packages will be installed: 180s autopkgtest-satdep cpl-plugin-muse libblas3 libcext0 libcfitsio10t64 180s libcplcore26 libcpldfs26 libcpldrs26 libcplui26 liberfa1 libfftw3-double3 180s libfftw3-single3 libgfortran5 libgomp1 libgsl27 libgslcblas0 libjs-jquery 180s libjs-jquery-hotkeys libjs-jquery-isonscreen libjs-jquery-metadata 180s libjs-jquery-tablesorter libjs-jquery-throttle-debounce libjs-sphinxdoc 180s libjs-underscore liblapack3 libwcs8 python3-astropy 180s python3-astropy-iers-data python3-coverage python3-cpl python3-dateutil 180s python3-erfa python3-hypothesis python3-iniconfig python3-numpy 180s python3-packaging python3-pluggy python3-ply python3-pytest 180s python3-pytest-arraydiff python3-pytest-astropy 180s python3-pytest-astropy-header python3-pytest-cov python3-pytest-doctestplus 180s python3-pytest-filter-subpackage python3-pytest-mock 180s python3-pytest-remotedata python3-sortedcontainers 180s 0 upgraded, 48 newly installed, 0 to remove and 0 not upgraded. 180s Need to get 21.2 MB/21.2 MB of archives. 180s After this operation, 95.8 MB of additional disk space will be used. 180s Get:1 /tmp/autopkgtest.4tWrNl/1-autopkgtest-satdep.deb autopkgtest-satdep ppc64el 0 [728 B] 181s Get:2 http://ftpmaster.internal/ubuntu noble/main ppc64el libjs-jquery all 3.6.1+dfsg+~3.5.14-1 [328 kB] 181s Get:3 http://ftpmaster.internal/ubuntu noble/universe ppc64el libjs-jquery-hotkeys all 0~20130707+git2d51e3a9+dfsg-2ubuntu2 [11.5 kB] 181s Get:4 http://ftpmaster.internal/ubuntu noble/universe ppc64el libcext0 ppc64el 7.3.2+ds-1build3 [43.3 kB] 181s Get:5 http://ftpmaster.internal/ubuntu noble/universe ppc64el libcfitsio10t64 ppc64el 4.3.1-1.1build2 [713 kB] 181s Get:6 http://ftpmaster.internal/ubuntu noble/main ppc64el libgomp1 ppc64el 14-20240412-0ubuntu1 [161 kB] 181s Get:7 http://ftpmaster.internal/ubuntu noble/main ppc64el libfftw3-double3 ppc64el 3.3.10-1ubuntu3 [443 kB] 181s Get:8 http://ftpmaster.internal/ubuntu noble/main ppc64el libfftw3-single3 ppc64el 3.3.10-1ubuntu3 [453 kB] 181s Get:9 http://ftpmaster.internal/ubuntu noble/universe ppc64el libcplcore26 ppc64el 7.3.2+ds-1build3 [656 kB] 181s Get:10 http://ftpmaster.internal/ubuntu noble/universe ppc64el libcplui26 ppc64el 7.3.2+ds-1build3 [42.7 kB] 181s Get:11 http://ftpmaster.internal/ubuntu noble/universe ppc64el libcpldfs26 ppc64el 7.3.2+ds-1build3 [47.1 kB] 181s Get:12 http://ftpmaster.internal/ubuntu noble/universe ppc64el libwcs8 ppc64el 8.2.2+ds-3build2 [342 kB] 181s Get:13 http://ftpmaster.internal/ubuntu noble/universe ppc64el libcpldrs26 ppc64el 7.3.2+ds-1build3 [78.5 kB] 182s Get:14 http://ftpmaster.internal/ubuntu noble-proposed/universe ppc64el libgslcblas0 ppc64el 2.7.1+dfsg-6ubuntu2 [86.6 kB] 182s Get:15 http://ftpmaster.internal/ubuntu noble-proposed/universe ppc64el libgsl27 ppc64el 2.7.1+dfsg-6ubuntu2 [1090 kB] 182s Get:16 http://ftpmaster.internal/ubuntu noble/universe ppc64el cpl-plugin-muse ppc64el 2.8.7+dfsg-3 [618 kB] 182s Get:17 http://ftpmaster.internal/ubuntu noble/main ppc64el libblas3 ppc64el 3.12.0-3build1 [227 kB] 182s Get:18 http://ftpmaster.internal/ubuntu noble/main ppc64el libgfortran5 ppc64el 14-20240412-0ubuntu1 [574 kB] 182s Get:19 http://ftpmaster.internal/ubuntu noble/universe ppc64el libjs-jquery-metadata all 12-4 [6582 B] 182s Get:20 http://ftpmaster.internal/ubuntu noble/universe ppc64el libjs-jquery-tablesorter all 1:2.31.3+dfsg1-3 [193 kB] 182s Get:21 http://ftpmaster.internal/ubuntu noble/universe ppc64el libjs-jquery-throttle-debounce all 1.1+dfsg.1-2 [12.5 kB] 182s Get:22 http://ftpmaster.internal/ubuntu noble/main ppc64el libjs-underscore all 1.13.4~dfsg+~1.11.4-3 [118 kB] 182s Get:23 http://ftpmaster.internal/ubuntu noble/main ppc64el libjs-sphinxdoc all 7.2.6-6 [149 kB] 182s Get:24 http://ftpmaster.internal/ubuntu noble/main ppc64el liblapack3 ppc64el 3.12.0-3build1 [2804 kB] 182s Get:25 http://ftpmaster.internal/ubuntu noble/universe ppc64el python3-iniconfig all 1.1.1-2 [6024 B] 182s Get:26 http://ftpmaster.internal/ubuntu noble/main ppc64el python3-packaging all 24.0-1 [41.1 kB] 182s Get:27 http://ftpmaster.internal/ubuntu noble/universe ppc64el python3-pluggy all 1.4.0-1 [20.4 kB] 182s Get:28 http://ftpmaster.internal/ubuntu noble/universe ppc64el python3-pytest all 7.4.4-1 [305 kB] 182s Get:29 http://ftpmaster.internal/ubuntu noble/main ppc64el python3-dateutil all 2.8.2-3ubuntu1 [79.4 kB] 182s Get:30 http://ftpmaster.internal/ubuntu noble/main ppc64el python3-sortedcontainers all 2.4.0-2 [27.6 kB] 182s Get:31 http://ftpmaster.internal/ubuntu noble/universe ppc64el python3-hypothesis all 6.98.15-1 [311 kB] 182s Get:32 http://ftpmaster.internal/ubuntu noble/main ppc64el python3-numpy ppc64el 1:1.26.4+ds-6ubuntu1 [4446 kB] 183s Get:33 http://ftpmaster.internal/ubuntu noble/universe ppc64el python3-pytest-arraydiff all 0.6.1-2 [10.2 kB] 183s Get:34 http://ftpmaster.internal/ubuntu noble/universe ppc64el python3-pytest-astropy-header all 0.2.2-1 [8190 B] 183s Get:35 http://ftpmaster.internal/ubuntu noble/universe ppc64el python3-coverage ppc64el 7.4.4+dfsg1-0ubuntu2 [149 kB] 183s Get:36 http://ftpmaster.internal/ubuntu noble/universe ppc64el libjs-jquery-isonscreen all 1.2.0-1.1 [3244 B] 183s Get:37 http://ftpmaster.internal/ubuntu noble/universe ppc64el python3-pytest-cov all 4.1.0-1 [21.5 kB] 183s Get:38 http://ftpmaster.internal/ubuntu noble/universe ppc64el python3-pytest-doctestplus all 1.2.0-1 [23.1 kB] 183s Get:39 http://ftpmaster.internal/ubuntu noble/universe ppc64el python3-pytest-filter-subpackage all 0.2.0-1 [6094 B] 183s Get:40 http://ftpmaster.internal/ubuntu noble/universe ppc64el python3-pytest-mock all 3.12.0-1.1 [11.3 kB] 183s Get:41 http://ftpmaster.internal/ubuntu noble/universe ppc64el python3-pytest-remotedata all 0.4.1-1 [8650 B] 183s Get:42 http://ftpmaster.internal/ubuntu noble/universe ppc64el python3-pytest-astropy all 0.11.0-1 [5902 B] 183s Get:43 http://ftpmaster.internal/ubuntu noble/main ppc64el python3-ply all 3.11-6 [46.5 kB] 183s Get:44 http://ftpmaster.internal/ubuntu noble/universe ppc64el python3-astropy-iers-data all 0.2024.01.01.00.33.39-1 [2046 kB] 183s Get:45 http://ftpmaster.internal/ubuntu noble/universe ppc64el liberfa1 ppc64el 2.0.1-1 [141 kB] 183s Get:46 http://ftpmaster.internal/ubuntu noble/universe ppc64el python3-erfa ppc64el 2.0.1.1+ds-3 [316 kB] 183s Get:47 http://ftpmaster.internal/ubuntu noble/universe ppc64el python3-astropy ppc64el 6.0.0-1ubuntu2 [3916 kB] 183s Get:48 http://ftpmaster.internal/ubuntu noble/universe ppc64el python3-cpl ppc64el 0.7.4-2build10 [35.7 kB] 184s Fetched 21.2 MB in 3s (7199 kB/s) 184s Selecting previously unselected package libjs-jquery. 184s (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 ... 71981 files and directories currently installed.) 184s Preparing to unpack .../00-libjs-jquery_3.6.1+dfsg+~3.5.14-1_all.deb ... 184s Unpacking libjs-jquery (3.6.1+dfsg+~3.5.14-1) ... 184s Selecting previously unselected package libjs-jquery-hotkeys. 184s Preparing to unpack .../01-libjs-jquery-hotkeys_0~20130707+git2d51e3a9+dfsg-2ubuntu2_all.deb ... 184s Unpacking libjs-jquery-hotkeys (0~20130707+git2d51e3a9+dfsg-2ubuntu2) ... 184s Selecting previously unselected package libcext0:ppc64el. 184s Preparing to unpack .../02-libcext0_7.3.2+ds-1build3_ppc64el.deb ... 184s Unpacking libcext0:ppc64el (7.3.2+ds-1build3) ... 184s Selecting previously unselected package libcfitsio10t64:ppc64el. 184s Preparing to unpack .../03-libcfitsio10t64_4.3.1-1.1build2_ppc64el.deb ... 184s Unpacking libcfitsio10t64:ppc64el (4.3.1-1.1build2) ... 184s Selecting previously unselected package libgomp1:ppc64el. 184s Preparing to unpack .../04-libgomp1_14-20240412-0ubuntu1_ppc64el.deb ... 184s Unpacking libgomp1:ppc64el (14-20240412-0ubuntu1) ... 184s Selecting previously unselected package libfftw3-double3:ppc64el. 184s Preparing to unpack .../05-libfftw3-double3_3.3.10-1ubuntu3_ppc64el.deb ... 184s Unpacking libfftw3-double3:ppc64el (3.3.10-1ubuntu3) ... 184s Selecting previously unselected package libfftw3-single3:ppc64el. 184s Preparing to unpack .../06-libfftw3-single3_3.3.10-1ubuntu3_ppc64el.deb ... 184s Unpacking libfftw3-single3:ppc64el (3.3.10-1ubuntu3) ... 184s Selecting previously unselected package libcplcore26:ppc64el. 184s Preparing to unpack .../07-libcplcore26_7.3.2+ds-1build3_ppc64el.deb ... 184s Unpacking libcplcore26:ppc64el (7.3.2+ds-1build3) ... 184s Selecting previously unselected package libcplui26:ppc64el. 184s Preparing to unpack .../08-libcplui26_7.3.2+ds-1build3_ppc64el.deb ... 184s Unpacking libcplui26:ppc64el (7.3.2+ds-1build3) ... 184s Selecting previously unselected package libcpldfs26:ppc64el. 184s Preparing to unpack .../09-libcpldfs26_7.3.2+ds-1build3_ppc64el.deb ... 184s Unpacking libcpldfs26:ppc64el (7.3.2+ds-1build3) ... 184s Selecting previously unselected package libwcs8:ppc64el. 184s Preparing to unpack .../10-libwcs8_8.2.2+ds-3build2_ppc64el.deb ... 184s Unpacking libwcs8:ppc64el (8.2.2+ds-3build2) ... 184s Selecting previously unselected package libcpldrs26:ppc64el. 184s Preparing to unpack .../11-libcpldrs26_7.3.2+ds-1build3_ppc64el.deb ... 184s Unpacking libcpldrs26:ppc64el (7.3.2+ds-1build3) ... 184s Selecting previously unselected package libgslcblas0:ppc64el. 184s Preparing to unpack .../12-libgslcblas0_2.7.1+dfsg-6ubuntu2_ppc64el.deb ... 184s Unpacking libgslcblas0:ppc64el (2.7.1+dfsg-6ubuntu2) ... 184s Selecting previously unselected package libgsl27:ppc64el. 184s Preparing to unpack .../13-libgsl27_2.7.1+dfsg-6ubuntu2_ppc64el.deb ... 184s Unpacking libgsl27:ppc64el (2.7.1+dfsg-6ubuntu2) ... 184s Selecting previously unselected package cpl-plugin-muse:ppc64el. 184s Preparing to unpack .../14-cpl-plugin-muse_2.8.7+dfsg-3_ppc64el.deb ... 184s Unpacking cpl-plugin-muse:ppc64el (2.8.7+dfsg-3) ... 184s Selecting previously unselected package libblas3:ppc64el. 184s Preparing to unpack .../15-libblas3_3.12.0-3build1_ppc64el.deb ... 184s Unpacking libblas3:ppc64el (3.12.0-3build1) ... 184s Selecting previously unselected package libgfortran5:ppc64el. 184s Preparing to unpack .../16-libgfortran5_14-20240412-0ubuntu1_ppc64el.deb ... 184s Unpacking libgfortran5:ppc64el (14-20240412-0ubuntu1) ... 184s Selecting previously unselected package libjs-jquery-metadata. 184s Preparing to unpack .../17-libjs-jquery-metadata_12-4_all.deb ... 184s Unpacking libjs-jquery-metadata (12-4) ... 184s Selecting previously unselected package libjs-jquery-tablesorter. 184s Preparing to unpack .../18-libjs-jquery-tablesorter_1%3a2.31.3+dfsg1-3_all.deb ... 184s Unpacking libjs-jquery-tablesorter (1:2.31.3+dfsg1-3) ... 184s Selecting previously unselected package libjs-jquery-throttle-debounce. 184s Preparing to unpack .../19-libjs-jquery-throttle-debounce_1.1+dfsg.1-2_all.deb ... 184s Unpacking libjs-jquery-throttle-debounce (1.1+dfsg.1-2) ... 184s Selecting previously unselected package libjs-underscore. 184s Preparing to unpack .../20-libjs-underscore_1.13.4~dfsg+~1.11.4-3_all.deb ... 184s Unpacking libjs-underscore (1.13.4~dfsg+~1.11.4-3) ... 184s Selecting previously unselected package libjs-sphinxdoc. 184s Preparing to unpack .../21-libjs-sphinxdoc_7.2.6-6_all.deb ... 184s Unpacking libjs-sphinxdoc (7.2.6-6) ... 184s Selecting previously unselected package liblapack3:ppc64el. 184s Preparing to unpack .../22-liblapack3_3.12.0-3build1_ppc64el.deb ... 184s Unpacking liblapack3:ppc64el (3.12.0-3build1) ... 184s Selecting previously unselected package python3-iniconfig. 184s Preparing to unpack .../23-python3-iniconfig_1.1.1-2_all.deb ... 184s Unpacking python3-iniconfig (1.1.1-2) ... 184s Selecting previously unselected package python3-packaging. 184s Preparing to unpack .../24-python3-packaging_24.0-1_all.deb ... 184s Unpacking python3-packaging (24.0-1) ... 184s Selecting previously unselected package python3-pluggy. 184s Preparing to unpack .../25-python3-pluggy_1.4.0-1_all.deb ... 184s Unpacking python3-pluggy (1.4.0-1) ... 184s Selecting previously unselected package python3-pytest. 184s Preparing to unpack .../26-python3-pytest_7.4.4-1_all.deb ... 184s Unpacking python3-pytest (7.4.4-1) ... 184s Selecting previously unselected package 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cpl-plugin-muse:ppc64el (2.8.7+dfsg-3) ... 191s Setting up python3-astropy (6.0.0-1ubuntu2) ... 195s Setting up python3-cpl (0.7.4-2build10) ... 195s Setting up autopkgtest-satdep (0) ... 195s Processing triggers for man-db (2.12.0-4build1) ... 195s Processing triggers for libc-bin (2.39-0ubuntu8) ... 199s (Reading database ... 75869 files and directories currently installed.) 199s Removing autopkgtest-satdep (0) ... 200s autopkgtest [23:48:37]: test test-recipe.py: [----------------------- 200s Recipe muse_scibasic: 200s version 2.8.7 200s 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} 200s Docstring: Remove the instrumental signature from the data of each CCD and 200s convert them from an image into a pixel table. 200s 200s Processing handles each raw input image separately: it trims the raw 200s data and records the overscan statistics, subtracts the bias (taking 200s account of the overscan, if --overscan is not "none"), optionally 200s detects cosmic rays (note that by default cosmic ray rejection is 200s handled in the post processing recipes while the data is reformatted 200s into a datacube, so that the default setting is cr="none" here), 200s converts the images from adu to count, subtracts the dark, divides by 200s the flat-field, and (optionally) propagates the integrated flux value 200s from the twilight-sky cube. The reduced image is then saved (if 200s --saveimage=true). The input calibrations geometry table, trace table, 200s and wavelength calibration table are used to assign 3D coordinates to 200s each CCD-based pixel, thereby creating a pixel table for each 200s exposure. If --skylines contains one or more wavelengths for (bright 200s and isolated) sky emission lines, these lines are used to correct the 200s wavelength calibration using an offset. The data is then cut to a 200s useful wavelength range (if --crop=true). If an ILLUM exposure was 200s given as input, it is then used to correct the relative illumination 200s between all slices of one IFU. For this, the data of each slice is 200s multiplied by the normalized median flux of that slice in the ILLUM 200s exposure. As last step, the data is divided by the normalized twilight 200s cube (if given), using the 3D coordinate of each pixel in the pixel 200s table to interpolate the twilight correction onto the data. This pre- 200s reduced pixel table for each exposure is then saved to disk. 200s 200s Parameters: 200s nifu: IFU to handle. If set to 0, all IFUs are processed 200s serially. If set to -1, all IFUs are processed in 200s parallel. (int; default: 0) 200s overscan: If this is "none", stop when detecting discrepant 200s overscan levels (see ovscsigma), for "offset" it 200s assumes that the mean overscan level represents the 200s real offset in the bias levels of the exposures 200s involved, and adjusts the data accordingly; for 200s "vpoly", a polynomial is fit to the vertical overscan 200s and subtracted from the whole quadrant. (str; default: 200s 'vpoly') 200s ovscreject: This influences how values are rejected when computing 200s overscan statistics. Either no rejection at all 200s ("none"), rejection using the DCR algorithm ("dcr"), or 200s rejection using an iterative constant fit ("fit"). 200s (str; default: 'dcr') 200s ovscsigma: If the deviation of mean overscan levels between a raw 200s input image and the reference image is higher than 200s |ovscsigma x stdev|, stop the processing. If 200s overscan="vpoly", this is used as sigma rejection level 200s for the iterative polynomial fit (the level comparison 200s is then done afterwards with |100 x stdev| to guard 200s against incompatible settings). Has no effect for 200s overscan="offset". (float; default: 30.0) 200s ovscignore: The number of pixels of the overscan adjacent to the 200s data section of the CCD that are ignored when computing 200s statistics or fits. (int; default: 3) 200s crop: Automatically crop the output pixel tables in 200s wavelength depending on the expected useful wavelength 200s range of the active instrument mode (4750-9350 Angstrom 200s for nominal mode and NFM, 4700-9350 Angstrom for 200s nominal AO mode, and 4600-9350 Angstrom for the 200s extended modes). (bool; default: True) 200s cr: Type of cosmic ray cleaning to use (for quick-look data 200s processing). (str; default: 'none') 200s xbox: Search box size in x. Only used if cr=dcr. (int; 200s default: 15) 200s ybox: Search box size in y. Only used if cr=dcr. (int; 200s default: 40) 200s passes: Maximum number of cleaning passes. Only used if cr=dcr. 200s (int; default: 2) 200s thres: Threshold for detection gap in factors of standard 200s deviation. Only used if cr=dcr. (float; default: 5.8) 200s combine: Type of combination to use. Note that in most cases, 200s science exposures cannot easily be combined on the CCD 200s level, so this should usually be kept as "none"! This 200s does not pay attention about the type of input data, 200s and will combine all raw inputs! (str; default: 'none') 200s nlow: Number of minimum pixels to reject with minmax (int; 200s default: 1) 200s nhigh: Number of maximum pixels to reject with minmax (int; 200s default: 1) 200s nkeep: Number of pixels to keep with minmax (int; default: 1) 200s lsigma: Low sigma for pixel rejection with sigclip (float; 200s default: 3.0) 200s hsigma: High sigma for pixel rejection with sigclip (float; 200s default: 3.0) 200s scale: Scale the individual images to a common exposure time 200s before combining them. (bool; default: True) 200s saveimage: Save the pre-processed CCD-based image of each input 200s exposure before it is transformed into a pixel table. 200s (bool; default: True) 200s skylines: List of wavelengths of sky emission lines (in Angstrom) 200s to use as reference for wavelength offset correction 200s using a Gaussian fit. It can contain multiple 200s (isolated) lines, as comma-separated list, individual 200s shifts are then combined into one weighted average 200s offset. Set to "none" to deactivate. (str; default: 200s '5577.339,6300.304') 200s skyhalfwidth: Half-width of the extraction box (in Angstrom) around 200s each sky emission line. (float; default: 5.0) 200s skybinsize: Size of the bins (in Angstrom per pixel) for the 200s intermediate spectrum to do the Gaussian fit to each 200s sky emission line. (float; default: 0.1) 200s skyreject: Sigma clipping parameters for the intermediate spectrum 200s to do the Gaussian fit to each sky emission line. Up to 200s three comma-separated numbers can be given, which are 200s interpreted as high sigma-clipping limit (float), low 200s limit (float), and number of iterations (integer), 200s respectively. (str; default: '15.,15.,1') 200s resample: Resample the input science data into 2D spectral images 200s using all supplied calibrations for a visual check. 200s Note that the image produced will show small wiggles 200s even when the input calibrations are good and were 200s applied successfully! (bool; default: False) 200s dlambda: Wavelength step (in Angstrom per pixel) to use for 200s resampling. (float; default: 1.25) 200s merge: Merge output products from different IFUs into a common 200s file. (bool; default: False) 200s 200s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 200s 'TRACE_TABLE', 'WAVECAL_TABLE', 'GEOMETRY_TABLE', 200s 'TWILIGHT_CUBE', 'BADPIX_TABLE'] 200s 200s Raw and product frames: 200s OBJECT --> ['OBJECT_RED', 'OBJECT_RESAMPLED', 'PIXTABLE_OBJECT'] 200s STD --> ['STD_RED', 'STD_RESAMPLED', 'PIXTABLE_STD'] 200s SKY --> ['SKY_RED', 'SKY_RESAMPLED', 'PIXTABLE_SKY'] 200s ASTROMETRY --> ['ASTROMETRY_RED', 'ASTROMETRY_RESAMPLED', 200s 'PIXTABLE_ASTROMETRY'] 200s ILLUM --> [] 200s REDUCED --> ['REDUCED_RESAMPLED', 'PIXTABLE_REDUCED'] 200s Author: Peter Weilbacher 200s 200s 200s Recipe muse_standard: 200s version 2.8.7 200s Parameters: {'profile': 'auto', 'select': 'distance', 'smooth': 'ppoly', 'lambdamin': 4000.0, 'lambdamax': 10000.0, 'lambdaref': 7000.0, 'darcheck': 'none', 'filter': 'white'} 200s Docstring: Create a flux response curve from a standard star exposure. 200s 200s Merge pixel tables from all IFUs and correct for differential 200s atmospheric refraction, when necessary. To derive the flux response 200s curve, integrate the flux of all objects detected within the field of 200s view using the given profile. Select one object as the standard star 200s (either the brightest or the one nearest one, depending on --select) 200s and compare its measured fluxes to tabulated fluxes to derive the 200s sensitivity over wavelength. Postprocess this sensitivity curve to 200s mark wavelength ranges affected by telluric absorption. Interpolate 200s over the telluric regions and derive a telluric correction spectrum 200s for them. The final response curve is then linearly extrapolated to 200s the largest possible MUSE wavelength range and smoothed (with the 200s method given by --smooth). The derivation of the telluric correction 200s spectrum assumes that the star has a smooth spectrum within the 200s telluric regions. If there are more than one exposure given in the 200s input data, the derivation of the flux response and telluric 200s corrections are done separately for each exposure. For each exposure, 200s an image containing the extracted stellar spectra and the datacube 200s used for flux integration are saved, together with collapsed images 200s for each given filter. In MUSE's WFM data (both AO and non-AO), the 200s Moffat profile is a good approximation of the actual PSF. Using the 200s smoothed profile ("smoffat") helps to increase the S/N and in most 200s cases removes systematics. In NFM, however, the profile is a 200s combination of a wide PSF plus the central AO-corrected peak, which 200s cannot be fit well by an analytical profile. In this case the circular 200s aperture is the best way to extract the flux. Using --profile="auto" 200s (the default) selects these options to give the best flux extraction 200s for most cases. 200s 200s Parameters: 200s profile: Type of flux integration to use. "gaussian", "moffat", and 200s "smoffat" use 2D profile fitting, "circle" and "square" 200s are non-optimal aperture flux integrators. "smoffat" uses 200s smoothing of the Moffat parameters from an initial fit, to 200s derive physically meaningful wavelength- dependent 200s behavior. "auto" selects the smoothed Moffat profile for 200s WFM data and circular flux integration for NFM. (str; 200s default: 'auto') 200s select: How to select the star for flux integration, "flux" uses 200s the brightest star in the field, "distance" uses the 200s detection nearest to the approximate coordinates of the 200s reference source. (str; default: 'distance') 200s smooth: How to smooth the response curve before writing it to 200s disk. "none" does not do any kind of smoothing (such a 200s response curve is only useful, if smoothed externally; 200s "median" does a median-filter of 15 Angstrom half-width; 200s "ppoly" fits piecewise cubic polynomials (each one across 200s 2x150 Angstrom width) postprocessed by a sliding average 200s filter of 15 Angstrom half-width. (str; default: 'ppoly') 200s lambdamin: Cut off the data below this wavelength after loading the 200s pixel table(s). (float; default: 4000.0) 200s lambdamax: Cut off the data above this wavelength after loading the 200s pixel table(s). (float; default: 10000.0) 200s lambdaref: Reference wavelength used for correction of differential 200s atmospheric refraction. The R-band (peak wavelength ~7000 200s Angstrom) that is usually used for guiding, is close to 200s the central wavelength of MUSE, so a value of 7000.0 200s Angstrom should be used if nothing else is known. A value 200s less than zero switches DAR correction off. (float; 200s default: 7000.0) 200s darcheck: Carry out a check of the theoretical DAR correction using 200s source centroiding. If "correct" it will also apply an 200s empirical correction. (str; default: 'none') 200s filter: The filter name(s) to be used for the output field-of-view 200s image. Each name has to correspond to an EXTNAME in an 200s extension of the FILTER_LIST file. If an unsupported 200s filter name is given, creation of the respective image is 200s omitted. If multiple filter names are given, they have to 200s be comma separated. If the zeropoint QC parameters are 200s wanted, make sure to add "Johnson_V,Cousins_R,Cousins_I". 200s (str; default: 'white') 200s 200s Calibration frames: ['EXTINCT_TABLE', 'STD_FLUX_TABLE', 200s 'TELLURIC_REGIONS', 'FILTER_LIST'] 200s 200s Raw and product frames: 200s PIXTABLE_STD --> ['DATACUBE_STD', 'STD_FLUXES', 'STD_RESPONSE', 200s 'STD_TELLURIC'] 200s Author: Peter Weilbacher 200s 200s 200s Recipe muse_bias: 200s version 2.8.7 200s 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} 200s Docstring: Combine several separate bias images into one master bias file. 200s 200s This recipe combines several separate bias images into one master bias 200s file. The master bias contains the combined pixel values, in adu, of 200s the raw bias exposures, with respect to the image combination method 200s used. Processing trims the raw data and records the overscan 200s statistics, corrects the data levels using the overscan (if overscan 200s is not "none") and combines the exposures using input parameters. The 200s read-out noise is computed for each quadrant of the raw input images 200s and stored as QC parameter. The variance extension is filled with an 200s initial value accordingly, before image combination. Further QC 200s statistics are computed on the output master bias. Additionally, bad 200s columns are searched for and marked in the data quality extension. 200s 200s Parameters: 200s nifu: IFU to handle. If set to 0, all IFUs are processed 200s serially. If set to -1, all IFUs are processed in 200s parallel. (int; default: 0) 200s overscan: If this is "none", stop when detecting discrepant 200s overscan levels (see ovscsigma), for "offset" it 200s assumes that the mean overscan level represents the 200s real offset in the bias levels of the exposures 200s involved, and adjusts the data accordingly; for 200s "vpoly", a polynomial is fit to the vertical overscan 200s and subtracted from the whole quadrant. (str; default: 200s 'vpoly') 200s ovscreject: This influences how values are rejected when computing 200s overscan statistics. Either no rejection at all 200s ("none"), rejection using the DCR algorithm ("dcr"), 200s or rejection using an iterative constant fit ("fit"). 200s (str; default: 'dcr') 200s ovscsigma: If the deviation of mean overscan levels between a raw 200s input image and the reference image is higher than 200s |ovscsigma x stdev|, stop the processing. If 200s overscan="vpoly", this is used as sigma rejection 200s level for the iterative polynomial fit (the level 200s comparison is then done afterwards with |100 x stdev| 200s to guard against incompatible settings). Has no effect 200s for overscan="offset". (float; default: 30.0) 200s ovscignore: The number of pixels of the overscan adjacent to the 200s data section of the CCD that are ignored when 200s computing statistics or fits. (int; default: 3) 200s combine: Type of image combination to use. (str; default: 200s 'sigclip') 200s nlow: Number of minimum pixels to reject with minmax. (int; 200s default: 1) 200s nhigh: Number of maximum pixels to reject with minmax. (int; 200s default: 1) 200s nkeep: Number of pixels to keep with minmax. (int; default: 200s 1) 200s lsigma: Low sigma for pixel rejection with sigclip. (float; 200s default: 3.0) 200s hsigma: High sigma for pixel rejection with sigclip. (float; 200s default: 3.0) 200s losigmabadpix: Low sigma to find dark columns in the combined bias 200s (float; default: 30.0) 200s hisigmabadpix: High sigma to find bright columns in the combined bias 200s (float; default: 3.0) 200s merge: Merge output products from different IFUs into a 200s common file. (bool; default: False) 200s 200s Calibration frames: ['BADPIX_TABLE'] 200s 200s Raw and product frames: 200s BIAS --> ['MASTER_BIAS'] 200s Author: Peter Weilbacher 200s 200s 200s Recipe muse_scipost_raman: 200s version 2.8.7 200s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'lambdaref': 7000.0, 'width': 20.0, 'crsigma': 15.0, 'fraction': 0.75, 'ignore': 0.05} 200s Docstring: Remove of 4GLSF Raman emission. 200s 200s This recipe removes the Raman scattered light of the 4GLSF system from 200s the exposure. It must be before the normal sky subtraction. 200s 200s Parameters: 200s lambdamin: Cut off the data below this wavelength after loading the 200s pixel table(s). (float; default: 4000.0) 200s lambdamax: Cut off the data above this wavelength after loading the 200s pixel table(s). (float; default: 10000.0) 200s lambdaref: Reference wavelength used for correction of differential 200s atmospheric refraction. The R-band (peak wavelength ~7000 200s Angstrom) that is usually used for guiding, is close to 200s the central wavelength of MUSE, so a value of 7000.0 200s Angstrom should be used if nothing else is known. A value 200s less than zero switches DAR correction off. (float; 200s default: 7000.0) 200s width: Wavelength range around Raman lines [Angstrom]. (float; 200s default: 20.0) 200s crsigma: Sigma level clipping for cube-based CR rejection (using 200s "median", see muse_scipost). It can be switched off, by 200s passing zero or a negative value. (float; default: 15.0) 200s fraction: Fraction of the image (without the ignored part) to be 200s considered as sky. If an input sky mask is provided, the 200s fraction is applied to the regions within the mask. If the 200s whole sky mask should be used, set this parameter to 1. 200s (float; default: 0.75) 200s ignore: Lowest fraction of the image to be ignored. If an input 200s sky mask is provided, the fraction is applied to the 200s regions within the mask. If the whole sky mask should be 200s used, set this parameter to 0. (float; default: 0.05) 200s 200s Calibration frames: ['RAMAN_LINES', 'LSF_PROFILE', 'SKY_MASK'] 200s 200s Raw and product frames: 200s PIXTABLE_OBJECT --> ['RAMAN_IMAGES', 'PIXTABLE_REDUCED'] 200s Author: Ole Streicher 200s 200s 200s Recipe muse_scipost_apply_astrometry: 200s version 2.8.7 200s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0} 200s Docstring: Calibrate astrometry for MUSE pixel tables. 200s 200s Apply an astrometric calibration to the pixel table spatial 200s coordinates. This is a task separated from muse_scipost. 200s 200s Parameters: 200s lambdamin: Cut off the data below this wavelength after loading the 200s pixel table(s). (float; default: 4000.0) 200s lambdamax: Cut off the data above this wavelength after loading the 200s pixel table(s). (float; default: 10000.0) 200s 200s Calibration frames: ['ASTROMETRY_WCS'] 200s 200s Raw and product frames: 200s PIXTABLE_OBJECT --> ['PIXTABLE_OBJECT'] 200s Author: Ole Streicher 200s 200s 200s Recipe muse_scipost_subtract_sky_simple: 200s version 2.8.7 200s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0} 200s Docstring: Subtract night sky spectrum. 200s 200s Subtract the sky in a simple way, just using a sky spectrum created by 200s muse_create_sky. This is a separated task of muse_scipost. 200s 200s Parameters: 200s lambdamin: Cut off the data below this wavelength after loading the 200s pixel table(s). (float; default: 4000.0) 200s lambdamax: Cut off the data above this wavelength after loading the 200s pixel table(s). (float; default: 10000.0) 200s 200s Calibration frames: ['SKY_SPECTRUM'] 200s 200s Raw and product frames: 200s PIXTABLE_REDUCED --> ['PIXTABLE_REDUCED'] 200s Author: Peter Weilbacher 200s 200s 200s Recipe muse_scipost_correct_rv: 200s version 2.8.7 200s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'rvcorr': 'bary'} 200s Docstring: Apply RV correction for MUSE pixel tables. 200s 200s Correct the wavelengths in the pixel table by given radial-velocity 200s correction. This is a task separated from muse_scipost. 200s 200s Parameters: 200s lambdamin: Cut off the data below this wavelength after loading the 200s pixel table(s). (float; default: 4000.0) 200s lambdamax: Cut off the data above this wavelength after loading the 200s pixel table(s). (float; default: 10000.0) 200s rvcorr: Correct the radial velocity of the telescope with 200s reference to either the barycenter of the Solar System 200s (bary), the center of the Sun (helio), or to the center of 200s the Earth (geo). (str; default: 'bary') 200s 200s Calibration frames: [] 200s 200s Raw and product frames: 200s PIXTABLE_OBJECT --> ['PIXTABLE_REDUCED'] 200s Author: Peter Weilbacher 200s 200s 200s Recipe muse_scipost: 200s version 2.8.7 200s 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} 200s Docstring: Prepare reduced and combined science products. 200s 200s Sort input pixel tables into lists of files per exposure, merge pixel 200s tables from all IFUs of each exposure. Correct each exposure for 200s differential atmospheric refraction (unless --lambdaref is far outside 200s the MUSE wavelength range, or NFM is used which has a built-in 200s corrector). Then the flux calibration is carried out, if a response 200s curve was given in the input; it includes a correction of telluric 200s absorption, if a telluric absorption correction file was given. If 200s observations were done with AO and a RAMAN_LINES file was given, a 200s procedure is run to clean the Raman scattering emission lines from the 200s data. Next, the slice autocalibration is computed and the flux 200s correction factors are applied to the pixel table (if 200s --autocalib="deepfield"). If user-provided autocalibration is 200s requested (--autocalib="user"), then the autocalibration is not 200s computed on the input exposure but the autocalibration factors are 200s read from the AUTOCAL_FACTORS table and applied directly to the data. 200s Then the sky subtraction is carried out (unless --skymethod="none"), 200s either directly subtracting an input sky continuum and an input sky 200s emission lines (for --skymethod="subtract-model"), or 200s (--skymethod="model") create a sky spectrum from the darkest fraction 200s (--skymodel_fraction, after ignoring the lowest --skymodel_ignore as 200s artifacts) of the field of view, then fitting and subtracting sky 200s emission lines using an initial estimate of the input sky lines; then 200s the continuum (residuals after subtracting the sky lines from the sky 200s spectrum) is subtracted as well. If --save contains "skymodel", all 200s sky-related products are saved for each exposure. Afterwards the data 200s is corrected for the radial velocity of the observer (--rvcorr), 200s before the input (or a default) astrometric solution is applied. Now 200s each individual exposure is fully reduced; the pixel tables at this 200s stage can be saved by setting "individual" in --save. If multiple 200s exposures were given, they are then combined. If --save contains 200s "combined", this final merged pixel table is saved. Finally (if --save 200s contains "cube"), the data is resampled into a datacube, using all 200s parameters given to the recipe. The extent and orientation of the cube 200s is normally computed from the data itself, but this can be overridden 200s by passing a file with the output world coordinate system 200s (OUTPUT_WCS), for example a MUSE cube. This can also be used to sample 200s the wavelength axis logarithmically (in that file set "CTYPE3='AWAV- 200s LOG'"). As a last step, the computed cube is integrated over all 200s filter functions given (--filter) that are also present in the input 200s filter list table. 200s 200s Parameters: 200s save: Select output product(s) to save. Can contain one 200s or more of "cube", "autocal", "skymodel", 200s "individual", "positioned", "combined", and 200s "stacked". If several options are given, they 200s have to be comma- separated. ("cube": output cube 200s and associated images, if this is not given, no 200s final resampling is done at all -- "autocal": up 200s to two additional output products related to the 200s slice autocalibration -- "raman": up to four 200s additional output products about the Raman light 200s distribution for AO observations -- "skymodel": 200s up to four additional output products about the 200s effectively used sky that was subtracted with the 200s "model" method -- "individual": fully reduced 200s pixel table for each individual exposure -- 200s "positioned": fully reduced and positioned pixel 200s table for each individual exposure, the 200s difference to "individual" is that here, the 200s output pixel tables have coordinates in RA and 200s DEC, and the optional offsets were applied; this 200s is only useful, if both the relative exposure 200s weighting and the final resampling are to be done 200s externally -- "combined": fully reduced and 200s combined pixel table for the full set of 200s exposures, the difference to "positioned" is that 200s all pixel tables are combined into one, with an 200s added weight column; this is useful, if only the 200s final resampling step is to be done separately -- 200s "stacked": an additional output file in form of a 200s 2D column-stacked image, i.e. x direction is 200s pseudo-spatial, y direction is wavelength.) (str; 200s default: 'cube,skymodel') 200s resample: The resampling technique to use for the final 200s output cube. (str; default: 'drizzle') 200s dx: Horizontal step size for resampling (in arcsec or 200s pixel). The following defaults are taken when 200s this value is set to 0.0: 0.2'' for WFM, 0.025'' 200s for NFM, 1.0 if data is in pixel units. (float; 200s default: 0.0) 200s dy: Vertical step size for resampling (in arcsec or 200s pixel). The following defaults are taken when 200s this value is set to 0.0: 0.2'' for WFM, 0.025'' 200s for NFM, 1.0 if data is in pixel units. (float; 200s default: 0.0) 200s dlambda: Wavelength step size (in Angstrom). Natural 200s instrument sampling is used, if this is 0.0 200s (float; default: 0.0) 200s crtype: Type of statistics used for detection of cosmic 200s rays during final resampling. "iraf" uses the 200s variance information, "mean" uses standard 200s (mean/stdev) statistics, "median" uses median and 200s the median median of the absolute median 200s deviation. (str; default: 'median') 200s crsigma: Sigma rejection factor to use for cosmic ray 200s rejection during final resampling. A zero or 200s negative value switches cosmic ray rejection off. 200s (float; default: 15.0) 200s rc: Critical radius for the "renka" resampling 200s method. (float; default: 1.25) 200s pixfrac: Pixel down-scaling factor for the "drizzle" 200s resampling method. Up to three, comma-separated, 200s floating-point values can be given. If only one 200s value is given, it applies to all dimensions, two 200s values are interpreted as spatial and spectral 200s direction, respectively, while three are taken as 200s horizontal, vertical, and spectral. (str; 200s default: '0.8,0.8') 200s ld: Number of adjacent pixels to take into account 200s during resampling in all three directions (loop 200s distance); this affects all resampling methods 200s except "nearest". (int; default: 1) 200s format: Type of output file format, "Cube" is a standard 200s FITS cube with NAXIS=3 and multiple extensions 200s (for data and variance). The extended "x" formats 200s include the reconstructed image(s) in FITS image 200s extensions within the same file. "sdpCube" does 200s some extra calculations to create FITS keywords 200s for the ESO Science Data Products. (str; default: 200s 'Cube') 200s weight: Type of weighting scheme to use when combining 200s multiple exposures. "exptime" just uses the 200s exposure time to weight the exposures, "fwhm" 200s uses the best available seeing information from 200s the headers as well, "none" preserves an existing 200s weight column in the input pixel tables without 200s changes. (str; default: 'exptime') 200s filter: The filter name(s) to be used for the output 200s field-of-view image. Each name has to correspond 200s to an EXTNAME in an extension of the FILTER_LIST 200s file. If an unsupported filter name is given, 200s creation of the respective image is omitted. If 200s multiple filter names are given, they have to be 200s comma separated. (str; default: 'white') 200s autocalib: The type of autocalibration to use. "none" 200s switches it off, "deepfield" uses the revised 200s MPDAF method that can be used for the reduction 200s of mostly empty "Deep Fields", "user" searches 200s for a user- provided table with autocalibration 200s factors. (str; default: 'none') 200s raman_width: Wavelength range around Raman lines [Angstrom]. 200s (float; default: 20.0) 200s skymethod: The method used to subtract the sky background 200s (spectrum). Option "model" should work in all 200s kinds of science fields: it uses a global sky 200s spectrum model with a local LSF. "model" uses 200s fluxes indicated in the SKY_LINES file as 200s starting estimates, but re-fits them on the 200s global sky spectrum created from the science 200s exposure. If SKY_CONTINUUM is given, it is 200s directly subtracted, otherwise it is created from 200s the sky region of the science exposure. Option 200s "subtract- model" uses the input SKY_LINES and 200s SKY_CONTINUUM, subtracting them directly without 200s re-fitting the fluxes, but still makes use of the 200s local LSF, hence LSF_PROFILE is required. The 200s inputs LSF_PROFILE and SKY_LINES are necessary 200s for these two model-based methods; SKY_CONTINUUM 200s is required for "subtract-model" and optional for 200s "model"; SKY_MASK is optional for "model". 200s Finally, option "simple" creates a sky spectrum 200s from the science data, and directly subtracts it, 200s without taking the LSF into account (LSF_PROFILE 200s and input SKY files are ignored). It works on 200s data that was not flux calibrated. (str; default: 200s 'model') 200s lambdamin: Cut off the data below this wavelength after 200s loading the pixel table(s). (float; default: 200s 4000.0) 200s lambdamax: Cut off the data above this wavelength after 200s loading the pixel table(s). (float; default: 200s 10000.0) 200s lambdaref: Reference wavelength used for correction of 200s differential atmospheric refraction. The R-band 200s (peak wavelength ~7000 Angstrom) that is usually 200s used for guiding, is close to the central 200s wavelength of MUSE, so a value of 7000.0 Angstrom 200s should be used if nothing else is known. A value 200s less than zero switches DAR correction off. 200s (float; default: 7000.0) 200s darcheck: Carry out a check of the theoretical DAR 200s correction using source centroiding. If "correct" 200s it will also apply an empirical correction. (str; 200s default: 'none') 200s skymodel_fraction: Fraction of the image (without the ignored part) 200s to be considered as sky. If an input sky mask is 200s provided, the fraction is applied to the regions 200s within the mask. If the whole sky mask should be 200s used, set this parameter to 1. (float; default: 200s 0.1) 200s skymodel_ignore: Fraction of the image to be ignored. If an input 200s sky mask is provided, the fraction is applied to 200s the regions within the mask. If the whole sky 200s mask should be used, set this parameter to 0. 200s (float; default: 0.05) 200s skymodel_sampling: Spectral sampling of the sky spectrum [Angstrom]. 200s (float; default: 0.3125) 200s skymodel_csampling: Spectral sampling of the continuum spectrum 200s [Angstrom]. (float; default: 0.3125) 200s sky_crsigma: Sigma level clipping for cube-based and spectrum- 200s based CR rejection when creating the sky 200s spectrum. This has to be a string of two comma- 200s separated floating-point numbers. The first value 200s gives the sigma- level rejection for cube-based 200s CR rejection (using "median"), the second value 200s the sigma-level for spectrum-based CR cleaning. 200s Both can be switched off, by passing zero or a 200s negative value. (str; default: '15.,15.') 200s rvcorr: Correct the radial velocity of the telescope with 200s reference to either the barycenter of the Solar 200s System (bary), the center of the Sun (helio), or 200s to the center of the Earth (geo). (str; default: 200s 'bary') 200s astrometry: If false, skip any astrometric calibration, even 200s if one was passed in the input set of files. This 200s causes creation of an output cube with a linear 200s WCS and may result in errors. If you want to use 200s a sensible default, leave this true but do not 200s pass an ASTROMETRY_WCS. (bool; default: True) 200s 200s Calibration frames: ['EXTINCT_TABLE', 'STD_RESPONSE', 'STD_TELLURIC', 200s 'ASTROMETRY_WCS', 'OFFSET_LIST', 'FILTER_LIST', 200s 'OUTPUT_WCS', 'AUTOCAL_FACTORS', 'RAMAN_LINES', 200s 'SKY_LINES', 'SKY_CONTINUUM', 'LSF_PROFILE', 200s 'SKY_MASK'] 200s 200s Raw and product frames: 200s PIXTABLE_OBJECT --> ['DATACUBE_FINAL', 'IMAGE_FOV', 200s 'OBJECT_RESAMPLED', 'PIXTABLE_REDUCED', 200s 'PIXTABLE_POSITIONED', 'PIXTABLE_COMBINED', 200s 'AUTOCAL_MASK', 'AUTOCAL_FACTORS', 200s 'RAMAN_IMAGES', 'SKY_IMAGE', 'SKY_MASK', 200s 'SKY_SPECTRUM', 'SKY_LINES', 'SKY_CONTINUUM'] 200s Author: Peter Weilbacher 200s 200s 200s Recipe muse_scipost_calibrate_flux: 200s version 2.8.7 200s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0} 200s Docstring: Calibrate flux for MUSE pixel tables. 200s 200s Replace the intensity in the MUSE pixel tables by the absolute flux. 200s This is a task separated from muse_scipost. 200s 200s Parameters: 200s lambdamin: Cut off the data below this wavelength after loading the 200s pixel table(s). (float; default: 4000.0) 200s lambdamax: Cut off the data above this wavelength after loading the 200s pixel table(s). (float; default: 10000.0) 200s 200s Calibration frames: ['EXTINCT_TABLE', 'STD_RESPONSE', 'STD_TELLURIC'] 200s 200s Raw and product frames: 200s PIXTABLE_OBJECT --> ['PIXTABLE_OBJECT'] 200s Author: Ole Streicher 200s 200s 200s Recipe muse_scipost_correct_dar: 200s version 2.8.7 200s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'lambdaref': 7000.0, 'darcheck': 'none'} 200s Docstring: Apply DAR correction for MUSE pixel tables. 200s 200s Correct the coordinates in the pixel table by differential atmospheric 200s refraction. This is a task separated from muse_scipost. 200s 200s Parameters: 200s lambdamin: Cut off the data below this wavelength after loading the 200s pixel table(s). (float; default: 4000.0) 200s lambdamax: Cut off the data above this wavelength after loading the 200s pixel table(s). (float; default: 10000.0) 200s lambdaref: Reference wavelength used for correction of differential 200s atmospheric refraction. The R-band (peak wavelength ~7000 200s Angstrom) that is usually used for guiding, is close to 200s the central wavelength of MUSE, so a value of 7000.0 200s Angstrom should be used if nothing else is known. A value 200s less than zero switches DAR correction off. (float; 200s default: 7000.0) 200s darcheck: Carry out a check of the theoretical DAR correction using 200s source centroiding. If "correct" it will also apply an 200s empirical correction. (str; default: 'none') 200s 200s Calibration frames: [] 200s 200s Raw and product frames: 200s PIXTABLE_OBJECT --> ['PIXTABLE_OBJECT'] 200s Author: Ole Streicher 200s 200s 200s Recipe muse_lsf: 200s version 2.8.7 200s 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'} 200s Docstring: Compute the LSF 200s 200s Compute the slice and wavelength dependent LSF from a lines spectrum 200s (ARC lamp). 200s 200s Parameters: 200s nifu: IFU to handle. If set to 0, all IFUs are 200s processed serially. If set to -1, all IFUs are 200s processed in parallel. (int; default: 0) 200s overscan: If this is "none", stop when detecting 200s discrepant overscan levels (see ovscsigma), 200s for "offset" it assumes that the mean overscan 200s level represents the real offset in the bias 200s levels of the exposures involved, and adjusts 200s the data accordingly; for "vpoly", a 200s polynomial is fit to the vertical overscan and 200s subtracted from the whole quadrant. (str; 200s default: 'vpoly') 200s ovscreject: This influences how values are rejected when 200s computing overscan statistics. Either no 200s rejection at all ("none"), rejection using the 200s DCR algorithm ("dcr"), or rejection using an 200s iterative constant fit ("fit"). (str; default: 200s 'dcr') 200s ovscsigma: If the deviation of mean overscan levels 200s between a raw input image and the reference 200s image is higher than |ovscsigma x stdev|, stop 200s the processing. If overscan="vpoly", this is 200s used as sigma rejection level for the 200s iterative polynomial fit (the level comparison 200s is then done afterwards with |100 x stdev| to 200s guard against incompatible settings). Has no 200s effect for overscan="offset". (float; default: 200s 30.0) 200s ovscignore: The number of pixels of the overscan adjacent 200s to the data section of the CCD that are 200s ignored when computing statistics or fits. 200s (int; default: 3) 200s save_subtracted: Save the pixel table after the LSF 200s subtraction. (bool; default: False) 200s line_quality: Minimal quality flag in line catalog for 200s selection (int; default: 3) 200s lsf_range: Wavelength window (half size) around each line 200s to estimate LSF (float; default: 7.5) 200s lsf_size: Image size in LSF direction (int; default: 200s 150) 200s lambda_size: Image size in line wavelength direction (int; 200s default: 30) 200s lsf_regression_window: Size of the regression window in LSF direction 200s (float; default: 0.7) 200s merge: Merge output products from different IFUs into 200s a common file. (bool; default: False) 200s combine: Type of lampwise image combination to use. 200s (str; default: 'sigclip') 200s method: LSF generation method. Depending on this 200s value, either an interpolated LSF cube is 200s created, or a table with the parameters of a 200s hermitean gaussian. (str; default: 200s 'interpolate') 200s 200s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 200s 'TRACE_TABLE', 'WAVECAL_TABLE', 'BADPIX_TABLE', 200s 'LINE_CATALOG'] 200s 200s Raw and product frames: 200s ARC --> ['LSF_PROFILE', 'PIXTABLE_SUBTRACTED'] 200s ARC_LSF --> ['LSF_PROFILE', 'PIXTABLE_SUBTRACTED'] 200s Author: Ole Streicher 200s 200s 200s Recipe muse_flat: 200s version 2.8.7 200s 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} 200s Docstring: Combine several separate flat images into one master flat file, trace 200s slice locations, and locate dark pixels. 200s 200s This recipe combines several separate flat-field images into one 200s master flat-field file and traces the location of the slices on the 200s CCD. The master flat contains the combined pixel values of the raw 200s flat exposures, with respect to the image combination method used, 200s normalized to the mean flux. The trace table contains polynomials 200s defining the location of the slices on the CCD. Processing trims the 200s raw data and records the overscan statistics, subtracts the bias 200s (taking account of the overscan, if --overscan is not "none"), and 200s optionally, the dark from each raw input image, converts them from adu 200s to count, scales them according to their exposure time, and combines 200s the exposures using input parameters. To trace the position of the 200s slices on the CCD, their edges are located using a threshold method. 200s The edge detection is repeated at given intervals thereby tracing the 200s central position (the mean of both edges) and width of each slit 200s vertically across the CCD. Deviant positions of detections on CCD rows 200s can be detected and excluded before fitting a polynomial to all 200s positions measured for one slice. The polynomial parameters for each 200s slice are saved in the output trace table. Finally, the area between 200s the now known slice edges is searched for dark (and bright) pixels, 200s using statistics in each row of the master flat. 200s 200s Parameters: 200s nifu: IFU to handle. If set to 0, all IFUs are processed 200s serially. If set to -1, all IFUs are processed in 200s parallel. (int; default: 0) 200s overscan: If this is "none", stop when detecting discrepant 200s overscan levels (see ovscsigma), for "offset" it 200s assumes that the mean overscan level represents the 200s real offset in the bias levels of the exposures 200s involved, and adjusts the data accordingly; for 200s "vpoly", a polynomial is fit to the vertical overscan 200s and subtracted from the whole quadrant. (str; default: 200s 'vpoly') 200s ovscreject: This influences how values are rejected when computing 200s overscan statistics. Either no rejection at all 200s ("none"), rejection using the DCR algorithm ("dcr"), 200s or rejection using an iterative constant fit ("fit"). 200s (str; default: 'dcr') 200s ovscsigma: If the deviation of mean overscan levels between a raw 200s input image and the reference image is higher than 200s |ovscsigma x stdev|, stop the processing. If 200s overscan="vpoly", this is used as sigma rejection 200s level for the iterative polynomial fit (the level 200s comparison is then done afterwards with |100 x stdev| 200s to guard against incompatible settings). Has no effect 200s for overscan="offset". (float; default: 30.0) 200s ovscignore: The number of pixels of the overscan adjacent to the 200s data section of the CCD that are ignored when 200s computing statistics or fits. (int; default: 3) 200s combine: Type of combination to use (str; default: 'sigclip') 200s nlow: Number of minimum pixels to reject with minmax (int; 200s default: 1) 200s nhigh: Number of maximum pixels to reject with minmax (int; 200s default: 1) 200s nkeep: Number of pixels to keep with minmax (int; default: 1) 200s lsigma: Low sigma for pixel rejection with sigclip (float; 200s default: 3.0) 200s hsigma: High sigma for pixel rejection with sigclip (float; 200s default: 3.0) 200s scale: Scale the individual images to a common exposure time 200s before combining them. (bool; default: True) 200s normalize: Normalize the master flat to the average flux (bool; 200s default: True) 200s trace: Trace the position of the slices on the master flat 200s (bool; default: True) 200s nsum: Number of lines over which to average when tracing 200s (int; default: 32) 200s order: Order of polynomial fit to the trace (int; default: 5) 200s edgefrac: Fractional change required to identify edge when 200s tracing (float; default: 0.5) 200s losigmabadpix: Low sigma to find dark pixels in the master flat 200s (float; default: 5.0) 200s hisigmabadpix: High sigma to find bright pixels in the master flat 200s (float; default: 5.0) 200s samples: Create a table containing all tracing sample points. 200s (bool; default: False) 200s merge: Merge output products from different IFUs into a 200s common file. (bool; default: False) 200s 200s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'BADPIX_TABLE'] 200s 200s Raw and product frames: 200s FLAT --> ['MASTER_FLAT', 'TRACE_TABLE', 'TRACE_SAMPLES'] 200s Author: Peter Weilbacher (based on Joris Gerssen's draft) 200s 200s 200s Recipe muse_twilight: 200s version 2.8.7 200s 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} 200s Docstring: Combine several twilight skyflats into one cube, compute correction 200s factors for each IFU, and create a smooth 3D illumination correction. 200s 200s Processing first handles each raw input image separately: it trims the 200s raw data and records the overscan statistics, subtracts the bias 200s (taking account of the overscan, if --overscan is not "none"), 200s converts the images from adu to count, subtracts the dark, divides by 200s the flat-field and combines all the exposures using input parameters. 200s The input calibrations geometry table, trace table, and wavelength 200s calibration table are used to assign 3D coordinates to each CCD-based 200s pixel, thereby creating a pixel table from the master sky-flat. These 200s pixel tables are then cut in wavelength using the --lambdamin and 200s --lambdamax parameters. The integrated flux in each IFU is computed as 200s the sum of the data in the pixel table, and saved in the header, to be 200s used later as estimate for the relative throughput of each IFU. If an 200s ILLUM exposure was given as input, it is then used to correct the 200s relative illumination between all slices of one IFU. For this, the 200s data of each slice within the pixel table of each IFU is multiplied by 200s the normalized median flux of that slice in the ILLUM exposure. The 200s pixel tables of all IFUs are then merged, using the integrated fluxes 200s as inverse scaling factors, and a cube is reconstructed from the 200s merged dataset, using given parameters. A white-light image is created 200s from the cube. This skyflat cube is then saved to disk, with the 200s white-light image as one extension. To construct a smooth 3D 200s illumination correction, the cube is post-processed in the following 200s way: the white-light image is used to create a mask of the illuminated 200s area. From this area, the optional vignetting mask is removed. The 200s smoothing is then computed for each plane of the cube: the illuminated 200s area is smoothed (by a 5x7 median filter), normalized, fit with a 2D 200s polynomial (of given polynomial orders), and normalized again. A 200s smooth white image is then created by collapsing the smooth cube. If a 200s vignetting mask was given or NFM data is processed, an area close to 200s the edge of the MUSE field is used to compute a 2D correction for the 200s vignetted area: the original unsmoothed white-light image is corrected 200s for large scale gradients by dividing it with the smooth white image. 200s The residuals in the edge area (as defined by the input mask or 200s hardcoded for NFM) are then smoothed using input parameters. This 200s smoothed vignetting correction is the multiplied onto each plane of 200s the smooth cube, normalizing each plane again. This twilight cube is 200s then saved to disk. 200s 200s Parameters: 200s overscan: If this is "none", stop when detecting discrepant 200s overscan levels (see ovscsigma), for "offset" it 200s assumes that the mean overscan level represents the 200s real offset in the bias levels of the exposures 200s involved, and adjusts the data accordingly; for 200s "vpoly", a polynomial is fit to the vertical overscan 200s and subtracted from the whole quadrant. (str; default: 200s 'vpoly') 200s ovscreject: This influences how values are rejected when computing 200s overscan statistics. Either no rejection at all 200s ("none"), rejection using the DCR algorithm ("dcr"), 200s or rejection using an iterative constant fit ("fit"). 200s (str; default: 'dcr') 200s ovscsigma: If the deviation of mean overscan levels between a raw 200s input image and the reference image is higher than 200s |ovscsigma x stdev|, stop the processing. If 200s overscan="vpoly", this is used as sigma rejection 200s level for the iterative polynomial fit (the level 200s comparison is then done afterwards with |100 x stdev| 200s to guard against incompatible settings). Has no effect 200s for overscan="offset". (float; default: 30.0) 200s ovscignore: The number of pixels of the overscan adjacent to the 200s data section of the CCD that are ignored when 200s computing statistics or fits. (int; default: 3) 200s combine: Type of combination to use (str; default: 'sigclip') 200s nlow: Number of minimum pixels to reject with minmax (int; 200s default: 1) 200s nhigh: Number of maximum pixels to reject with minmax (int; 200s default: 1) 200s nkeep: Number of pixels to keep with minmax (int; default: 1) 200s lsigma: Low sigma for pixel rejection with sigclip (float; 200s default: 3.0) 200s hsigma: High sigma for pixel rejection with sigclip (float; 200s default: 3.0) 200s scale: Scale the individual images to a common exposure time 200s before combining them. (bool; default: False) 200s resample: The resampling technique to use for the final output 200s cube. (str; default: 'drizzle') 200s crtype: Type of statistics used for detection of cosmic rays 200s during final resampling. "iraf" uses the variance 200s information, "mean" uses standard (mean/stdev) 200s statistics, "median" uses median and the median median 200s of the absolute median deviation. (str; default: 200s 'median') 200s crsigma: Sigma rejection factor to use for cosmic ray rejection 200s during final resampling. A zero or negative value 200s switches cosmic ray rejection off. (float; default: 200s 50.0) 200s lambdamin: Minimum wavelength for twilight reconstruction. 200s (float; default: 5000.0) 200s lambdamax: Maximum wavelength for twilight reconstruction. 200s (float; default: 9000.0) 200s dlambda: Sampling for twilight reconstruction, this should 200s result in planes of equal wavelength coverage. (float; 200s default: 250.0) 200s xorder: Polynomial order to use in x direction to fit the full 200s field of view. (int; default: 2) 200s yorder: Polynomial order to use in y direction to fit the full 200s field of view. (int; default: 2) 200s vignmaskedges: Pixels on edges stronger than this fraction in the 200s normalized image are excluded from the fit to the 200s vignetted area. Set to non-positive number to include 200s them in the fit. This has no effect for NFM skyflats. 200s (float; default: 0.02) 200s vignsmooth: Type of smoothing to use for the vignetted region 200s given by the VIGNETTING_MASK (for WFM, or the internal 200s mask, for NFM); gaussian uses (vignxpar + vignypar)/2 200s as FWHM. (str; default: 'polyfit') 200s vignxpar: Parameter used by the vignetting smoothing: x order 200s for polyfit (default, recommended 4), parameter that 200s influences the FWHM for the gaussian (recommended: 200s 10), or x dimension of median filter (recommended 5). 200s If a negative value is found, the default is taken. 200s (int; default: -1) 200s vignypar: Parameter used by the vignetting smoothing: y order 200s for polyfit (default, recommended 4), parameter that 200s influences the FWHM for the gaussian (recommended: 200s 10), or y dimension of median filter (recommended 5). 200s If a negative value is found, the default is taken. 200s (int; default: -1) 200s vignnfmmask: The height of the vignetted region at the top of the 200s MUSE field in NFM. This is the region modeled 200s separately (the final vignetting model might be 200s smaller). (int; default: 22) 200s 200s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 200s 'BADPIX_TABLE', 'TRACE_TABLE', 'WAVECAL_TABLE', 200s 'GEOMETRY_TABLE', 'VIGNETTING_MASK'] 200s 200s Raw and product frames: 200s SKYFLAT --> ['DATACUBE_SKYFLAT', 'TWILIGHT_CUBE'] 200s ILLUM --> [] 200s Author: Peter Weilbacher 200s 200s 200s Recipe muse_ampl: 200s version 2.8.7 200s 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} 200s Docstring: Determine the instrumental throughput from exposures taken with the 200s pico-amplifier / photo diode readings. 200s 200s This recipe combines several separate amplifier images (flat-fields 200s with special FITS headers containing pico amplifier measurements) into 200s one master image file and computes the instrumental throughput per IFU 200s (and slice). Processing trims the raw data and records the overscan 200s statistics, subtracts the bias (taking account of the overscan, if 200s overscan is not "none"), and optionally, the dark from each raw input 200s image, converts them from adu to count, scales them according to their 200s exposure time, and combines them using input parameters. To compute 200s the throughput the image is converted into a pixel table, the flux is 200s then integrated over the given filter band, and the ratio of the 200s expected flux (FITS header INS.AMPL2.CURR) to measured flux is taken, 200s in the same units. If a geometry table was given as input, the 200s relative area of the IFUs is taken into account when computing the 200s flux per unit area. The resulting ratio is the instrument efficiency 200s (throughput) and saved as QC parameters for the whole input image and 200s per slice in the output pixel table. 200s 200s Parameters: 200s nifu: IFU to handle. If set to 0, all IFUs are processed 200s serially. If set to -1, all IFUs are processed in 200s parallel. (int; default: 0) 200s overscan: If this is "none", stop when detecting discrepant 200s overscan levels (see ovscsigma), for "offset" it assumes 200s that the mean overscan level represents the real offset 200s in the bias levels of the exposures involved, and adjusts 200s the data accordingly; for "vpoly", a polynomial is fit to 200s the vertical overscan and subtracted from the whole 200s quadrant. (str; default: 'vpoly') 200s ovscreject: This influences how values are rejected when computing 200s overscan statistics. Either no rejection at all ("none"), 200s rejection using the DCR algorithm ("dcr"), or rejection 200s using an iterative constant fit ("fit"). (str; default: 200s 'dcr') 200s ovscsigma: If the deviation of mean overscan levels between a raw 200s input image and the reference image is higher than 200s |ovscsigma x stdev|, stop the processing. If 200s overscan="vpoly", this is used as sigma rejection level 200s for the iterative polynomial fit (the level comparison is 200s then done afterwards with |100 x stdev| to guard against 200s incompatible settings). Has no effect for 200s overscan="offset". (float; default: 30.0) 200s ovscignore: The number of pixels of the overscan adjacent to the data 200s section of the CCD that are ignored when computing 200s statistics or fits. (int; default: 3) 200s combine: Type of combination to use (str; default: 'sigclip') 200s nlow: Number of minimum pixels to reject with minmax (int; 200s default: 1) 200s nhigh: Number of maximum pixels to reject with minmax (int; 200s default: 1) 200s nkeep: Number of pixels to keep with minmax (int; default: 1) 200s lsigma: Low sigma for pixel rejection with sigclip (float; 200s default: 3.0) 200s hsigma: High sigma for pixel rejection with sigclip (float; 200s default: 3.0) 200s fbeam: Factor to describe the widening of the beam from the 200s focal plane to photo diode 2. (float; default: 1.1) 200s temp: Lamp temperature [K] used to create the black body 200s function. (float; default: 3200.0) 200s savemaster: Save the processed and combined master image before any 200s concolution is done. (bool; default: False) 200s savetable: Save the table with all the processed pixel values. 200s (bool; default: False) 200s merge: Merge output products from different IFUs into a common 200s file. (bool; default: False) 200s 200s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'BADPIX_TABLE', 200s 'GEOMETRY_TABLE', 'FILTER_LIST', 'TRACE_TABLE', 200s 'WAVECAL_TABLE'] 200s 200s Raw and product frames: 200s AMPL --> ['MASTER_AMPL', 'TABLE_AMPL', 'AMPL_CONVOLVED'] 200s Author: Peter Weilbacher 200s 200s 200s Recipe muse_lingain: 200s version 2.8.7 200s 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} 200s Docstring: Compute the gain and a model of the residual non-linearity for each 200s detector quadrant 200s 200s The recipe uses the bias and flat field images of a detector 200s monitoring exposure sequence to determine the detector gain in 200s counts/ADU and to model the residual non-linearity for each of the 200s four detector quadrants of all IFUs. All measurements done by the 200s recipe are done on the illuminated parts of the detector, i.e. on the 200s slices. The location of the slices is taken from the given trace 200s table, which is a mandatory input. Using the traces of the slices on 200s the detector a set of measurement windows is placed along these 200s traces. The data used for the determination of the gain and the 200s residual non-linearity is the taken from these windows. Bad pixels 200s indicated by an, optionally, provided bad pixel table, or flagged 200s during the preprocessing (bias subtraction) of the input data are 200s excluded from the measurements. Local measurements of the read-out- 200s noise, the signal and the gain are calculated for each of the 200s measurement windows. Using these measurements the gain for each 200s detector quadrant is computed as the zero-order coefficient of a 1st 200s order polynomial fitted to the binned gain measurements as a function 200s of the signal level. The residual non-linearity is modelled by a 200s (high) order polynomial which is fitted to the fractional percentage 200s deviation of the count rate from an expected constant count rate (the 200s linear case) as function of the signal level. (Not yet implemented!) 200s 200s Parameters: 200s nifu: IFU to handle. If set to 0, all IFUs are processed 200s serially. If set to -1, all IFUs are processed in 200s parallel. (int; default: 0) 200s ybox: Size of windows along the traces of the slices. (int; 200s default: 50) 200s xgap: Extra offset from tracing edge. (int; default: 3) 200s xborder: Extra offset from the detector edge used for the selection 200s of slices. (int; default: 10) 200s order: Order of the polynomial used to fit the non-linearity 200s residuals. (int; default: 12) 200s toffset: Exposure time offset in seconds to apply to linearity flat 200s fields. (float; default: 0.018) 200s fluxtol: Tolerance value for the overall flux consistency check of 200s a pair of flat fields. The value is the maximum relative 200s offset. (float; default: 0.01) 200s sigma: Sigma value used for signal value clipping. (float; 200s default: 3.0) 200s signalmin: Minimum signal value in log(ADU) used for the gain 200s analysis and the non-linearity polynomial model. (float; 200s default: 0.0) 200s signalmax: Maximum signal value in log(ADU) used for the gain 200s analysis and the non-linearity polynomial model. (float; 200s default: 4.9) 200s signalbin: Size of a signal bin in log10(ADU) used for the gain 200s analysis and the non-linearity polynomial model. (float; 200s default: 0.1) 200s gainlimit: Minimum signal value [ADU] used for fitting the gain 200s relation. (float; default: 100.0) 200s gainsigma: Sigma value for gain value clipping. (float; default: 3.0) 200s ctsmin: Minimum signal value in log(counts) to consider for the 200s non-linearity analysis. (float; default: 3.0) 200s ctsmax: Maximum signal value in log(counts) to consider for the 200s non-linearity analysis. (float; default: 4.9) 200s ctsbin: Size of a signal bin in log10(counts) used for the non- 200s linearity analysis. (float; default: 0.1) 200s linearmin: Lower limit of desired linear range in log10(counts). 200s (float; default: 2.5) 200s linearmax: Upper limit of desired linear range in log10(counts). 200s (float; default: 3.0) 200s merge: Merge output products from different IFUs into a common 200s file. (bool; default: False) 200s 200s Calibration frames: ['MASTER_BIAS', 'TRACE_TABLE', 'BADPIX_TABLE'] 200s 200s Raw and product frames: 200s LINGAIN_LAMP_OFF --> ['NONLINEARITY_GAIN'] 200s LINGAIN_LAMP_ON --> ['NONLINEARITY_GAIN'] 200s Author: Ralf Palsa 200s 200s 200s Recipe muse_scipost_subtract_sky: 200s version 2.8.7 200s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'orig': '', 'flux_sky': 0.0, 'flux_lamp': 0.0} 200s Docstring: Subtract night sky model. 200s 200s Subtract the sky as defined by the sky lines and continuum from a 200s pixel table. This is a separated task of muse_scipost. 200s 200s Parameters: 200s lambdamin: Cut off the data below this wavelength after loading the 200s pixel table(s). (float; default: 4000.0) 200s lambdamax: Cut off the data above this wavelength after loading the 200s pixel table(s). (float; default: 10000.0) 200s orig: If specified, write an additional column containing the 200s original data to the pixel table. (str; default: '') 200s flux_sky: Reference flat field flux, obtained by sky exposure. This 200s parameter is needed to scale the data of each pixel table 200s if more than one pixel table was used to determine the 200s sky. By default, it is taken from the parameter ESO DRS 200s MUSE FLAT FLUX SKY of the first pixel table. (float; 200s default: 0.0) 200s flux_lamp: Reference flat field flux, obtained by lamp exposure. This 200s parameter is needed to scale the data of each pixel table 200s if more than one pixel table was used to determine the 200s sky. By default, it is taken from the parameter ESO DRS 200s MUSE FLAT FLUX LAMP of the first pixel table. (float; 200s default: 0.0) 200s 200s Calibration frames: ['SKY_LINES', 'SKY_CONTINUUM', 'LSF_PROFILE'] 200s 200s Raw and product frames: 200s PIXTABLE_REDUCED --> ['PIXTABLE_REDUCED'] 200s Author: Ole Streicher 200s 200s 200s Recipe muse_scipost_make_cube: 200s version 2.8.7 200s 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'} 200s Docstring: Make a MUSE cube from a MUSE pixel table. 200s 200s This recipe takes a pixel table and resamples it to either a FITS cube 200s or a Euro3D table and optionally to a stacked spectrum. This is a part 200s of the muse_scipost recipe. 200s 200s Parameters: 200s lambdamin: Cut off the data below this wavelength after loading the 200s pixel table(s). (float; default: 4000.0) 200s lambdamax: Cut off the data above this wavelength after loading the 200s pixel table(s). (float; default: 10000.0) 200s resample: The resampling technique to use for the final output cube. 200s (str; default: 'drizzle') 200s dx: Horizontal step size for resampling (in arcsec or pixel). 200s The following defaults are taken when this value is set to 200s 0.0: 0.2'' for WFM, 0.025'' for NFM, 1.0 if data is in 200s pixel units. (float; default: 0.0) 200s dy: Vertical step size for resampling (in arcsec or pixel). 200s The following defaults are taken when this value is set to 200s 0.0: 0.2'' for WFM, 0.025'' for NFM, 1.0 if data is in 200s pixel units. (float; default: 0.0) 200s dlambda: Wavelength step size (in Angstrom). Natural instrument 200s sampling is used, if this is 0.0 (float; default: 0.0) 200s crtype: Type of statistics used for detection of cosmic rays 200s during final resampling. "iraf" uses the variance 200s information, "mean" uses standard (mean/stdev) statistics, 200s "median" uses median and the median median of the absolute 200s median deviation. (str; default: 'median') 200s crsigma: Sigma rejection factor to use for cosmic ray rejection 200s during final resampling. A zero or negative value switches 200s cosmic ray rejection off. (float; default: 15.0) 200s rc: Critical radius for the "renka" resampling method. (float; 200s default: 1.25) 200s pixfrac: Pixel down-scaling factor for the "drizzle" resampling 200s method. Up to three, comma-separated, floating-point 200s values can be given. If only one value is given, it 200s applies to all dimensions, two values are interpreted as 200s spatial and spectral direction, respectively, while three 200s are taken as horizontal, vertical, and spectral. (str; 200s default: '0.8,0.8') 200s ld: Number of adjacent pixels to take into account during 200s resampling in all three directions (loop distance); this 200s affects all resampling methods except "nearest". (int; 200s default: 1) 200s format: Type of output file format, "Cube" is a standard FITS cube 200s with NAXIS=3 and multiple extensions (for data and 200s variance). The extended "x" formats include the 200s reconstructed image(s) in FITS image extensions within the 200s same file. (str; default: 'Cube') 200s stacked: If true, write an additional output file in form of a 2D 200s stacked image (x direction is pseudo-spatial, y direction 200s is wavelength). (bool; default: False) 200s filter: The filter name(s) to be used for the output field-of-view 200s image. Each name has to correspond to an EXTNAME in an 200s extension of the FILTER_LIST file. If an unsupported 200s filter name is given, creation of the respective image is 200s omitted. If multiple filter names are given, they have to 200s be comma separated. (str; default: 'white') 200s 200s Calibration frames: ['FILTER_LIST', 'OUTPUT_WCS'] 200s 200s Raw and product frames: 200s PIXTABLE_OBJECT --> ['DATACUBE_FINAL', 'IMAGE_FOV', 200s 'OBJECT_RESAMPLED'] 200s Author: Ole Streicher 200s 200s 200s Recipe muse_exp_align: 200s version 2.8.7 200s 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} 200s Docstring: Create a coordinate offset table to be used to align exposures during 200s exposure combination. 200s 200s Compute the coordinate offset for each input field-of-view image with 200s respect to a reference. The created list of coordinate offsets can 200s then be used in muse_exp_combine as the field coordinate offsets to 200s properly align the exposures during their combination. The source 200s positions used to compute the field offsets are obtained by detecting 200s point sources in each of the input images, unless the source detection 200s is overridden and an input source list is available for each input 200s field-of-view image. In this latter case the input source positions 200s are used to calculate the field offsets. 200s 200s Parameters: 200s rsearch: Search radius (in arcsec) for each iteration of 200s the offset computation. (str; default: 200s '30.,4.,2.,0.8') 200s nbins: Number of bins to use for 2D histogram on the 200s first iteration of the offset computation. (int; 200s default: 60) 200s weight: Use weighting. (bool; default: True) 200s fwhm: FWHM in pixels of the convolution filter. (float; 200s default: 5.0) 200s threshold: Initial intensity threshold for detecting point 200s sources. If the value is negative or zero the 200s threshold is taken as sigma above median 200s background MAD. If it is larger than zero the 200s threshold is taken as absolute background level. 200s (float; default: 15.0) 200s bkgignore: Fraction of the image to be ignored. (float; 200s default: 0.05) 200s bkgfraction: Fraction of the image (without the ignored part) 200s to be considered as background. (float; default: 200s 0.1) 200s step: Increment/decrement of the threshold value in 200s subsequent iterations. (float; default: 0.5) 200s iterations: Maximum number of iterations used for detecting 200s sources. (int; default: 100000) 200s srcmin: Minimum number of sources which must be found. 200s (int; default: 5) 200s srcmax: Maximum number of sources which may be found. 200s (int; default: 80) 200s roundmin: Lower limit of the allowed point-source 200s roundness. (float; default: -1.0) 200s roundmax: Upper limit of the allowed point-source 200s roundness. (float; default: 1.0) 200s sharpmin: Lower limit of the allowed point-source 200s sharpness. (float; default: 0.2) 200s sharpmax: Upper limit of the allowed point-source 200s sharpness. (float; default: 1.0) 200s expmap: Enables the creation of a simple exposure map for 200s the combined field- of-view. (bool; default: 200s False) 200s bpixdistance: Minimum allowed distance of a source to the 200s closest bad pixel in pixel. Detected sources 200s which are closer to a bad pixel are not taken 200s into account when computing the field offsets. 200s This option has no effect if the source positions 200s are taken from input catalogs. (float; default: 200s 5.0) 200s override_detection: Overrides the source detection step. If this is 200s enabled and source catalogs are present in the 200s input data set, the source positions used to 200s calculate the field offsets are read from the 200s input catalogs. If no catalogs are available as 200s input data the source positions are detected on 200s the input images. (bool; default: False) 200s 200s Calibration frames: ['SOURCE_LIST'] 200s 200s Raw and product frames: 200s IMAGE_FOV --> ['EXPOSURE_MAP', 'PREVIEW_FOV', 'SOURCE_LIST', 200s 'OFFSET_LIST'] 200s Author: Ralf Palsa 200s 200s 200s Recipe muse_exp_combine: 200s version 2.8.7 200s 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} 200s Docstring: Combine several exposures into one datacube. 200s 200s Sort reduced pixel tables, one per exposure, by exposure and combine 200s them with applied weights into one final datacube. 200s 200s Parameters: 200s save: Select output product(s) to save. Can contain one or more 200s of "cube" (output cube and associated images; if this is 200s not given, no resampling is done at all) or "combined" 200s (fully reduced and combined pixel table for the full set 200s of exposures; this is useful, if the final resampling step 200s is to be done again separately). If several options are 200s given, they have to be comma-separated. (str; default: 200s 'cube') 200s resample: The resampling technique to use for the final output cube. 200s (str; default: 'drizzle') 200s dx: Horizontal step size for resampling (in arcsec or pixel). 200s The following defaults are taken when this value is set to 200s 0.0: 0.2'' for WFM, 0.025'' for NFM, 1.0 if data is in 200s pixel units. (float; default: 0.0) 200s dy: Vertical step size for resampling (in arcsec or pixel). 200s The following defaults are taken when this value is set to 200s 0.0: 0.2'' for WFM, 0.025'' for NFM, 1.0 if data is in 200s pixel units. (float; default: 0.0) 200s dlambda: Wavelength step size (in Angstrom). Natural instrument 200s sampling is used, if this is 0.0 (float; default: 0.0) 200s crtype: Type of statistics used for detection of cosmic rays 200s during final resampling. "iraf" uses the variance 200s information, "mean" uses standard (mean/stdev) statistics, 200s "median" uses median and the median median of the absolute 200s median deviation. (str; default: 'median') 200s crsigma: Sigma rejection factor to use for cosmic ray rejection 200s during final resampling. A zero or negative value switches 200s cosmic ray rejection off. (float; default: 10.0) 200s rc: Critical radius for the "renka" resampling method. (float; 200s default: 1.25) 200s pixfrac: Pixel down-scaling factor for the "drizzle" resampling 200s method. Up to three, comma-separated, floating-point 200s values can be given. If only one value is given, it 200s applies to all dimensions, two values are interpreted as 200s spatial and spectral direction, respectively, while three 200s are taken as horizontal, vertical, and spectral. (str; 200s default: '0.6,0.6') 200s ld: Number of adjacent pixels to take into account during 200s resampling in all three directions (loop distance); this 200s affects all resampling methods except "nearest". (int; 200s default: 1) 200s format: Type of output file format, "Cube" is a standard FITS cube 200s with NAXIS=3 and multiple extensions (for data and 200s variance). The extended "x" formats include the 200s reconstructed image(s) in FITS image extensions within the 200s same file. "sdpCube" does some extra calculations to 200s create FITS keywords for the ESO Science Data Products. 200s (str; default: 'Cube') 200s weight: Type of weighting scheme to use when combining multiple 200s exposures. "exptime" just uses the exposure time to weight 200s the exposures, "fwhm" uses the best available seeing 200s information from the headers as well, "header" queries 200s ESO.DRS.MUSE.WEIGHT of each input file instead of the 200s FWHM, and "none" preserves an existing weight column in 200s the input pixel tables without changes. (str; default: 200s 'exptime') 200s filter: The filter name(s) to be used for the output field-of-view 200s image. Each name has to correspond to an EXTNAME in an 200s extension of the FILTER_LIST file. If an unsupported 200s filter name is given, creation of the respective image is 200s omitted. If multiple filter names are given, they have to 200s be comma separated. (str; default: 'white') 200s lambdamin: Cut off the data below this wavelength after loading the 200s pixel table(s). (float; default: 4000.0) 200s lambdamax: Cut off the data above this wavelength after loading the 200s pixel table(s). (float; default: 10000.0) 200s 200s Calibration frames: ['OFFSET_LIST', 'FILTER_LIST', 'OUTPUT_WCS'] 200s 200s Raw and product frames: 200s PIXTABLE_REDUCED --> ['DATACUBE_FINAL', 'IMAGE_FOV', 200s 'PIXTABLE_COMBINED'] 200s Author: Peter Weilbacher 200s 200s 200s Recipe muse_create_sky: 200s version 2.8.7 200s 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} 200s Docstring: Create night sky model from selected pixels of an exposure of empty 200s sky. 200s 200s This recipe creates the continuum and the atmospheric transition line 200s spectra of the night sky from the data in a pixel table(s) belonging 200s to one exposure of (mostly) empty sky. 200s 200s Parameters: 200s fraction: Fraction of the image (without the ignored part) to be 200s considered as sky. If an input sky mask is provided, the 200s fraction is applied to the regions within the mask. If the 200s whole sky mask should be used, set this parameter to 1. 200s (float; default: 0.75) 200s ignore: Fraction of the image to be ignored. If an input sky mask 200s is provided, the fraction is applied to the regions within 200s the mask. If the whole sky mask should be used, set this 200s parameter to 0. (float; default: 0.05) 200s sampling: Spectral sampling of the sky spectrum [Angstrom]. (float; 200s default: 0.3125) 200s csampling: Spectral sampling of the continuum spectrum [Angstrom]. 200s (float; default: 0.3125) 200s crsigma: Sigma level clipping for cube-based and spectrum-based CR 200s rejection. This has to be a string of two comma-separated 200s floating-point numbers. The first value gives the sigma- 200s level rejection for cube-based CR rejection (using 200s "median", see muse_scipost), the second value the sigma- 200s level for spectrum-based CR cleaning. Both can be switched 200s off, by passing zero or a negative value. (str; default: 200s '15.,15.') 200s lambdamin: Cut off the data below this wavelength after loading the 200s pixel table(s). (float; default: 4000.0) 200s lambdamax: Cut off the data above this wavelength after loading the 200s pixel table(s). (float; default: 10000.0) 200s lambdaref: Reference wavelength used for correction of differential 200s atmospheric refraction. The R-band (peak wavelength ~7000 200s Angstrom) that is usually used for guiding, is close to 200s the central wavelength of MUSE, so a value of 7000.0 200s Angstrom should be used if nothing else is known. A value 200s less than zero switches DAR correction off. (float; 200s default: 7000.0) 200s 200s Calibration frames: ['EXTINCT_TABLE', 'STD_RESPONSE', 'STD_TELLURIC', 200s 'SKY_LINES', 'SKY_CONTINUUM', 'LSF_PROFILE', 200s 'SKY_MASK'] 200s 200s Raw and product frames: 200s PIXTABLE_SKY --> ['SKY_MASK', 'SKY_IMAGE', 'SKY_SPECTRUM', 200s 'SKY_LINES', 'SKY_CONTINUUM'] 200s Author: Ole Streicher 200s 200s 200s Recipe muse_qi_mask: 200s version 2.8.7 200s Parameters: {'nifu': 0} 200s Docstring: Create image masks for use with the quick image reconstruction. 200s 200s Trace and wavelength calibration tables (24 of them each, one per IFU) 200s are used to build wavelength maps. If the input data is binned, the 200s wavelength maps are binned in the same way (averaging of pixels). The 200s wavelength maps are then thresholded to create masks of the desired 200s wavelength range. Finally, the mask is "untrimmed", i.e. empty regions 200s for the pre- and overscans are added (in a simple way, assuming 200s quadrants of equal size, and padding of 32 pixels on all quadrant 200s edges). Note: this recipe is not part of the main MUSE pipeline but to 200s be used in the integration phase to create image masks until the 200s system is fully qualified. It therefore does only minimal error 200s checking. 200s 200s Parameters: 200s nifu: IFU to handle. If set to 0, all IFUs are processed serially, 200s which is the recommendation for this recipe, since only then 200s all extensions end up in the same output file. (int; default: 200s 0) 200s 200s Calibration frames: ['TRACE_TABLE', 'WAVECAL_TABLE'] 200s 200s Raw and product frames: 200s BIAS --> ['MASK_IMAGE'] 200s Author: Peter Weilbacher 200s 200s 200s Recipe muse_illum: 200s version 2.8.7 200s Parameters: {} 200s Docstring: Dummy recipe to convert a raw illumination flat field into a DFS 200s product 200s 200s The recipe copies the data of an illumination flat-field unmodified to 200s the output file. However it alters the header data such that the 200s result is a DFS compliant product file, which can be used in the on- 200s line pipeline environment to correct the illumination of twilight 200s and/or science observations. This recipe has no use in any environment 200s other than the on-line pipeline environment! 200s 200s No parameters 200s Calibration frames: [] 200s 200s Raw and product frames: 200s ILLUMFLAT --> ['ILLUM'] 200s Author: Ralf Palsa 200s 200s 200s Recipe muse_astrometry: 200s version 2.8.7 200s 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'} 200s Docstring: Compute an astrometric solution. 200s 200s Merge pixel tables from all IFUs, apply correction for differential 200s atmospheric refraction (when necessary), optionally apply flux 200s calibration and telluric correction (if the necessary input data was 200s given), and resample the data from all exposures into a datacube. Use 200s the cube to detect objects which are then matched to their reference 200s positions from which a two-dimensional WCS solution is computed. There 200s are two pattern matching algorithm implemented, which can be selected 200s by chosing a positive or zero value of faccuracy. In the first method 200s (with a positive value of faccuracy), start using the search radius, 200s and iteratively decrease it, until no duplicate detections are 200s identified any more. Similarly, iterate the data accuracy (decrease it 200s downwards from the mean positioning error) until matches are found. 200s Remove the remaining unidentified objects. The second method (when 200s faccuracy is set to zero), iterates through all quadruples in both the 200s detected objects and the catalogue, calculates the transformation and 200s checks whether more than 80% of the detections match a catalog entry 200s within the radius. The main output is the ASTROMETRY_WCS file which is 200s a bare FITS header containing the world coordinate solution. The 200s secondary product is DATACUBE_ASTROMETRY, it is not needed for further 200s processing but can be used for verification and debugging. It contains 200s the reconstructed cube and two images created from it in further FITS 200s extensions: a white-light image and the special image created from the 200s central planes of the cube used to detect and centroid the stars (as 200s well as its variance). 200s 200s Parameters: 200s centroid: Centroiding method to use for objects in the field of 200s view. "gaussian" and "moffat" use 2D fits to derive the 200s centroid, "box" is a simple centroid in a square box. 200s (str; default: 'moffat') 200s detsigma: Source detection sigma level to use. If this is negative, 200s values between its absolute and 1.0 are tested with a 200s stepsize of 0.1, to find an optimal solution. (float; 200s default: 1.5) 200s radius: Initial radius in pixels for pattern matching 200s identification in the astrometric field. (float; default: 200s 3.0) 200s faccuracy: Factor of initial accuracy relative to mean positional 200s accuracy of the measured positions to use for pattern 200s matching. If this is set to zero, use the quadruples based 200s method. (float; default: 0.0) 200s niter: Number of iterations of the astrometric fit. (int; 200s default: 2) 200s rejsigma: Rejection sigma level of the astrometric fit. (float; 200s default: 3.0) 200s rotcenter: Center of rotation of the instrument, given as two comma- 200s separated floating point values in pixels. (str; default: 200s '-0.01,-1.20') 200s lambdamin: Cut off the data below this wavelength after loading the 200s pixel table(s). (float; default: 4000.0) 200s lambdamax: Cut off the data above this wavelength after loading the 200s pixel table(s). (float; default: 10000.0) 200s lambdaref: Reference wavelength used for correction of differential 200s atmospheric refraction. The R-band (peak wavelength ~7000 200s Angstrom) that is usually used for guiding, is close to 200s the central wavelength of MUSE, so a value of 7000.0 200s Angstrom should be used if nothing else is known. A value 200s less than zero switches DAR correction off. (float; 200s default: 7000.0) 200s darcheck: Carry out a check of the theoretical DAR correction using 200s source centroiding. If "correct" it will also apply an 200s empirical correction. (str; default: 'none') 200s 200s Calibration frames: ['ASTROMETRY_REFERENCE', 'EXTINCT_TABLE', 200s 'STD_RESPONSE', 'STD_TELLURIC'] 200s 200s Raw and product frames: 200s PIXTABLE_ASTROMETRY --> ['DATACUBE_ASTROMETRY', 'ASTROMETRY_WCS'] 200s Author: Peter Weilbacher 200s 200s 200s Recipe muse_geometry: 200s version 2.8.7 200s Parameters: {'ifu1': 1, 'ifu2': 24, 'sigma': 2.2, 'centroid': 'gaussian', 'smooth': 1.5, 'lambdamin': 6800.0, 'lambdamax': 7200.0} 200s Docstring: Compute relative location of the slices within the field of view and 200s measure the instrumental PSF on the detectors. 200s 200s Processing first works separately on each IFU of the raw input data 200s (in parallel): it trims the raw data and records the overscan 200s statistics, subtracts the bias and converts them from adu to count. 200s Optionally, the dark can be subtracted and the data can be divided by 200s the flat-field. The data of all input mask exposures is then averaged. 200s The averaged image together with the trace table and wavelength 200s calibration as well as the line catalog are used to detect spots. The 200s detection windows are used to measure the spots on all images of the 200s sequence, the result is saved, with information on the measured PSF, 200s in the spots tables. Then properties of all slices are computed, first 200s separately on each IFU to determine the peak position of the mask for 200s each slice and its angle, subsequently the width and horizontal 200s position. Then, the result of all IFUs is analyzed together to produce 200s a refined horizontal position, applying global shifts to each IFU as 200s needed. The vertical position is then determined using the known slice 200s ordering on the sky; the relative peak positions are put into 200s sequence, taking into account the vertical offsets of the pinholes in 200s the mask. The table is then cleaned up from intermediate debug data. 200s If the --smooth parameter is set to a positive value, it is used to do 200s a sigma-clipped smoothing within each slicer stack, for a more regular 200s appearance of the output table. The table is then saved. As a last 200s optional step, additional raw input data is reduced using the newly 200s geometry to produce an image of the field of view. If these exposures 200s contain smooth features, they can be used as a visual check of the 200s quality of the geometrical calibration. 200s 200s Parameters: 200s ifu1: First IFU to analyze. (int; default: 1) 200s ifu2: Last IFU to analyze. (int; default: 24) 200s sigma: Sigma detection level for spot detection, in terms of 200s median deviation above the median. (float; default: 2.2) 200s centroid: Type of centroiding and FWHM determination to use for all 200s spot measurements: simple barycenter method or using a 200s Gaussian fit. (str; default: 'gaussian') 200s smooth: Use this sigma-level cut for smoothing of the output table 200s within each slicer stack. Set to non-positive value to 200s deactivate smoothing. (float; default: 1.5) 200s lambdamin: When passing any MASK_CHECK frames in the input, use this 200s lower wavelength cut before reconstructing the image. 200s (float; default: 6800.0) 200s lambdamax: When passing any MASK_CHECK frames in the input, use this 200s upper wavelength cut before reconstructing the image. 200s (float; default: 7200.0) 200s 200s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 200s 'TRACE_TABLE', 'WAVECAL_TABLE', 'LINE_CATALOG', 200s 'BADPIX_TABLE', 'MASK_CHECK'] 200s 200s Raw and product frames: 200s MASK --> ['MASK_REDUCED', 'MASK_COMBINED', 'SPOTS_TABLE', 200s 'GEOMETRY_UNSMOOTHED', 'GEOMETRY_TABLE', 'GEOMETRY_CUBE'] 200s Author: Peter Weilbacher 200s 200s 200s Recipe muse_scipost_combine_pixtables: 200s version 2.8.7 200s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'weight': 'exptime'} 200s Docstring: Combine MUSE pixel tables, either from different IFUs, or from 200s different exposures, or both. 200s 200s Sort pixel tables by exposure and combine them with applied weights 200s into one big pixel table. This is a task separated from muse_scipost. 200s 200s Parameters: 200s lambdamin: Cut off the data below this wavelength after loading the 200s pixel table(s). (float; default: 4000.0) 200s lambdamax: Cut off the data above this wavelength after loading the 200s pixel table(s). (float; default: 10000.0) 200s weight: Type of weighting scheme to use when combining multiple 200s exposures. "exptime" just uses the exposure time to weight 200s the exposures, "fwhm" uses the DIMM information in the 200s header as well, "none" preserves an existing weight column 200s in the input pixel tables without changes. (str; default: 200s 'exptime') 200s 200s Calibration frames: ['OFFSET_LIST'] 200s 200s Raw and product frames: 200s PIXTABLE_OBJECT --> ['PIXTABLE_COMBINED'] 200s Author: Ole Streicher 200s 200s 200s Recipe muse_wavecal: 200s version 2.8.7 200s 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} 200s Docstring: Detect arc emission lines and determine the wavelength solution for 200s each slice. 200s 200s This recipe detects arc emission lines and fits a wavelength solution 200s to each slice of the instrument. The wavelength calibration table 200s contains polynomials defining the wavelength solution of the slices on 200s the CCD. Processing trims the raw data and records the overscan 200s statistics, subtracts the bias (taking account of the overscan, if 200s --overscan is not "none") and converts them from adu to count. 200s Optionally, the dark can be subtracted and the data can be divided by 200s the flat-field, but this is not recommended. The data is then combined 200s using input parameters, into separate images for each lamp. To compute 200s the wavelength solution, arc lines are detected at the center of each 200s slice (using threshold detection on a S/N image) and subsequently 200s assigned wavelengths, using pattern matching to identify lines from 200s the input line catalog. Each line is then traced to the edges of the 200s slice, using Gaussian centering in each CCD column. The Gaussians not 200s only yield center, but also centering error, and line properties (e.g. 200s FWHM). Deviant fits are detected using polynomial fits to each arc 200s line (using the xorder parameter) and rejected. These analysis and 200s measuring steps are carried out separately on images exposed by the 200s different arc lamps, reducing the amount of blending, that can 200s otherwise influence line identification and Gaussian centering. The 200s final two-dimensional fit uses all positions (of all lamps), their 200s wavelengths, and the given polynomial orders to compute the final 200s wavelength solution for each slice, iteratively rejecting outliers. 200s This final fit can be either unweighted (fitweighting="uniform", for 200s fastest processing) or weighted (other values of fitweighting, for 200s higher accuracy). 200s 200s Parameters: 200s nifu: IFU to handle. If set to 0, all IFUs are processed 200s serially. If set to -1, all IFUs are processed in 200s parallel. (int; default: 0) 200s overscan: If this is "none", stop when detecting discrepant 200s overscan levels (see ovscsigma), for "offset" it 200s assumes that the mean overscan level represents the 200s real offset in the bias levels of the exposures 200s involved, and adjusts the data accordingly; for 200s "vpoly", a polynomial is fit to the vertical overscan 200s and subtracted from the whole quadrant. (str; default: 200s 'vpoly') 200s ovscreject: This influences how values are rejected when computing 200s overscan statistics. Either no rejection at all 200s ("none"), rejection using the DCR algorithm ("dcr"), or 200s rejection using an iterative constant fit ("fit"). 200s (str; default: 'dcr') 200s ovscsigma: If the deviation of mean overscan levels between a raw 200s input image and the reference image is higher than 200s |ovscsigma x stdev|, stop the processing. If 200s overscan="vpoly", this is used as sigma rejection level 200s for the iterative polynomial fit (the level comparison 200s is then done afterwards with |100 x stdev| to guard 200s against incompatible settings). Has no effect for 200s overscan="offset". (float; default: 30.0) 200s ovscignore: The number of pixels of the overscan adjacent to the 200s data section of the CCD that are ignored when computing 200s statistics or fits. (int; default: 3) 200s combine: Type of lampwise image combination to use. (str; 200s default: 'sigclip') 200s lampwise: Identify and measure the arc emission lines on images 200s separately for each lamp setup. (bool; default: True) 200s sigma: Sigma level used to detect arc emission lines above the 200s median background level in the S/N image of the central 200s column of each slice (float; default: 1.0) 200s dres: The allowed range of resolutions for pattern matching 200s (of detected arc lines to line list) in fractions 200s relative to the expected value (float; default: 0.05) 200s tolerance: Tolerance for pattern matching (of detected arc lines 200s to line list) (float; default: 0.1) 200s xorder: Order of the polynomial for the horizontal curvature 200s within each slice (int; default: 2) 200s yorder: Order of the polynomial used to fit the dispersion 200s relation (int; default: 6) 200s linesigma: Sigma level for iterative rejection of deviant fits for 200s each arc line within each slice, a negative value means 200s to use the default (2.5). (float; default: -1.0) 200s residuals: Create a table containing residuals of the fits to the 200s data of all arc lines. This is useful to assess the 200s quality of the wavelength solution in detail. (bool; 200s default: False) 200s fitsigma: Sigma level for iterative rejection of deviant 200s datapoints during the final polynomial wavelength 200s solution within each slice, a negative value means to 200s use the default (3.0). (float; default: -1.0) 200s fitweighting: Type of weighting to use in the final polynomial 200s wavelength solution fit, using centroiding error 200s estimate and/or scatter of each single line as 200s estimates of its accuracy. (str; default: 200s 'cerrscatter') 200s saveimages: Save (bool; default: False) 200s resample: Resample the input arc images onto 2D images for a 200s visual check using tracing and wavelength calibration 200s solutions. Note that the image produced will show small 200s wiggles even when the calibration was successful! 200s (bool; default: False) 200s wavemap: Create a wavelength map of the input images (bool; 200s default: False) 200s merge: Merge output products from different IFUs into a common 200s file. (bool; default: False) 200s 200s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 200s 'TRACE_TABLE', 'LINE_CATALOG', 'BADPIX_TABLE'] 200s 200s Raw and product frames: 200s ARC --> ['WAVECAL_TABLE', 'WAVECAL_RESIDUALS', 'ARC_RED_LAMP'] 200s Author: Peter Weilbacher 200s 200s 200s Recipe muse_dark: 200s version 2.8.7 200s 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} 201s Docstring: Combine several separate dark images into one master dark file and 201s locate hot pixels. 201s 201s This recipe combines several separate dark images into one master dark 201s file. The master dark contains the combined pixel values of the raw 201s dark exposures, with respect to the image combination method used and 201s normalization time specified. Processing trims the raw data and 201s records the overscan statistics, subtracts the bias (taking account of 201s the overscan, if --overscan is not "none") from each raw input image, 201s converts them from adu to count, scales them according to their 201s exposure time, and combines them using input parameters. Hot pixels 201s are then identified using image statistics and marked in the data 201s quality extension. The combined image is normalized to 1 hour exposure 201s time. QC statistics are computed on the output master dark. If 201s --model=true, a smooth polynomial model of the combined master dark is 201s computed, created from several individual 2D polynomials to describe 201s different features visible in MUSE dark frames. It is only advisable 201s to use this, if the master dark is the result of at least 50 201s individual long dark exposures. 201s 201s Parameters: 201s nifu: IFU to handle. If set to 0, all IFUs are processed 201s serially. If set to -1, all IFUs are processed in 201s parallel. (int; default: 0) 201s overscan: If this is "none", stop when detecting discrepant 201s overscan levels (see ovscsigma), for "offset" it assumes 201s that the mean overscan level represents the real offset 201s in the bias levels of the exposures involved, and adjusts 201s the data accordingly; for "vpoly", a polynomial is fit to 201s the vertical overscan and subtracted from the whole 201s quadrant. (str; default: 'vpoly') 201s ovscreject: This influences how values are rejected when computing 201s overscan statistics. Either no rejection at all ("none"), 201s rejection using the DCR algorithm ("dcr"), or rejection 201s using an iterative constant fit ("fit"). (str; default: 201s 'dcr') 201s ovscsigma: If the deviation of mean overscan levels between a raw 201s input image and the reference image is higher than 201s |ovscsigma x stdev|, stop the processing. If 201s overscan="vpoly", this is used as sigma rejection level 201s for the iterative polynomial fit (the level comparison is 201s then done afterwards with |100 x stdev| to guard against 201s incompatible settings). Has no effect for 201s overscan="offset". (float; default: 30.0) 201s ovscignore: The number of pixels of the overscan adjacent to the data 201s section of the CCD that are ignored when computing 201s statistics or fits. (int; default: 3) 201s combine: Type of image combination to use. (str; default: 201s 'sigclip') 201s nlow: Number of minimum pixels to reject with minmax. (int; 201s default: 1) 201s nhigh: Number of maximum pixels to reject with minmax. (int; 201s default: 1) 201s nkeep: Number of pixels to keep with minmax. (int; default: 1) 201s lsigma: Low sigma for pixel rejection with sigclip. (float; 201s default: 3.0) 201s hsigma: High sigma for pixel rejection with sigclip. (float; 201s default: 3.0) 201s scale: Scale the individual images to a common exposure time 201s before combining them. (bool; default: True) 201s normalize: Normalize the master dark to this exposure time (in 201s seconds). To disable normalization, set this to a 201s negative value. (float; default: 3600.0) 201s hotsigma: Sigma level, in terms of median deviation above the 201s median dark level, above which a pixel is detected and 201s marked as 'hot'. (float; default: 5.0) 201s model: Model the master dark using a set of polynomials. (bool; 201s default: False) 201s merge: Merge output products from different IFUs into a common 201s file. (bool; default: False) 201s 201s Calibration frames: ['MASTER_BIAS', 'BADPIX_TABLE'] 201s 201s Raw and product frames: 201s DARK --> ['MASTER_DARK', 'MODEL_DARK'] 201s Author: Peter Weilbacher 201s 201s 201s autopkgtest [23:48:38]: test test-recipe.py: -----------------------] 202s autopkgtest [23:48:39]: test test-recipe.py: - - - - - - - - - - results - - - - - - - - - - 202s test-recipe.py PASS (superficial) 202s autopkgtest [23:48:39]: @@@@@@@@@@@@@@@@@@@@ summary 202s test-recipe.py PASS (superficial) 215s Creating nova instance adt-noble-ppc64el-cpl-plugin-muse-20240418-234516-juju-7f2275-prod-proposed-migration-environment-2-469103a9-8abd-4ed9-8266-b58b69860d31 from image adt/ubuntu-noble-ppc64el-server-20240418.img (UUID eb57e9e5-70fe-4878-ae85-dd88e864cb24)...