0s autopkgtest [00:34:45]: starting date and time: 2024-04-19 00:34:45+0000 0s autopkgtest [00:34:45]: git checkout: 43bc6cdf gitlab-ci: do not include the salsa pipeline 0s autopkgtest [00:34:45]: host juju-7f2275-prod-proposed-migration-environment-3; command line: /home/ubuntu/autopkgtest/runner/autopkgtest --output-dir /tmp/autopkgtest-work.67096p32/out --timeout-copy=6000 --setup-commands /home/ubuntu/autopkgtest-cloud/worker-config-production/setup-canonical.sh --apt-pocket=proposed=src:gsl --apt-upgrade cpl-plugin-muse --timeout-short=300 --timeout-copy=20000 --timeout-build=20000 --env=ADT_TEST_TRIGGERS=gsl/2.7.1+dfsg-6ubuntu2 -- ssh -s /home/ubuntu/autopkgtest/ssh-setup/nova -- --flavor autopkgtest --security-groups autopkgtest-juju-7f2275-prod-proposed-migration-environment-3@bos01-s390x-13.secgroup --name adt-noble-s390x-cpl-plugin-muse-20240419-003444-juju-7f2275-prod-proposed-migration-environment-3-da439567-7fe6-4862-95ea-6619021587c3 --image adt/ubuntu-noble-s390x-server --keyname testbed-juju-7f2275-prod-proposed-migration-environment-3 --net-id=net_prod-proposed-migration -e TERM=linux -e ''"'"'http_proxy=http://squid.internal:3128'"'"'' -e ''"'"'https_proxy=http://squid.internal:3128'"'"'' -e ''"'"'no_proxy=127.0.0.1,127.0.1.1,login.ubuntu.com,localhost,localdomain,novalocal,internal,archive.ubuntu.com,ports.ubuntu.com,security.ubuntu.com,ddebs.ubuntu.com,changelogs.ubuntu.com,launchpadlibrarian.net,launchpadcontent.net,launchpad.net,10.24.0.0/24,keystone.ps5.canonical.com,objectstorage.prodstack5.canonical.com'"'"'' --mirror=http://us.ports.ubuntu.com/ubuntu-ports/ 170s autopkgtest [00:37:35]: testbed dpkg architecture: s390x 170s autopkgtest [00:37:35]: testbed apt version: 2.7.14build2 170s autopkgtest [00:37:35]: @@@@@@@@@@@@@@@@@@@@ test bed setup 170s Get:1 http://ftpmaster.internal/ubuntu noble-proposed InRelease [117 kB] 171s Get:2 http://ftpmaster.internal/ubuntu noble-proposed/restricted Sources [12.2 kB] 171s Get:3 http://ftpmaster.internal/ubuntu noble-proposed/multiverse Sources [2340 B] 171s Get:4 http://ftpmaster.internal/ubuntu noble-proposed/universe Sources [376 kB] 171s Get:5 http://ftpmaster.internal/ubuntu noble-proposed/main Sources [54.2 kB] 171s Get:6 http://ftpmaster.internal/ubuntu noble-proposed/main s390x Packages [95.6 kB] 171s Get:7 http://ftpmaster.internal/ubuntu noble-proposed/main s390x c-n-f Metadata [3032 B] 171s Get:8 http://ftpmaster.internal/ubuntu noble-proposed/restricted s390x Packages [976 B] 171s Get:9 http://ftpmaster.internal/ubuntu noble-proposed/restricted s390x c-n-f Metadata [116 B] 171s Get:10 http://ftpmaster.internal/ubuntu noble-proposed/universe s390x Packages [497 kB] 172s Get:11 http://ftpmaster.internal/ubuntu noble-proposed/universe s390x c-n-f Metadata [7292 B] 172s Get:12 http://ftpmaster.internal/ubuntu noble-proposed/multiverse s390x c-n-f Metadata [116 B] 173s Fetched 1166 kB in 2s (702 kB/s) 173s Reading package lists... 175s sh: 4: dhclient: not found 176s Reading package lists... 176s Building dependency tree... 176s Reading state information... 176s Calculating upgrade... 176s The following packages will be upgraded: 176s apport apport-core-dump-handler libkeyutils1 libnuma1 make man-db 176s netcat-openbsd numactl python3-apport python3-problem-report 176s 10 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 176s Need to get 1783 kB of archives. 176s After this operation, 3072 B disk space will be freed. 176s Get:1 http://ftpmaster.internal/ubuntu noble/main s390x python3-problem-report all 2.28.1-0ubuntu1 [23.8 kB] 176s Get:2 http://ftpmaster.internal/ubuntu noble/main s390x python3-apport all 2.28.1-0ubuntu1 [92.1 kB] 176s Get:3 http://ftpmaster.internal/ubuntu noble/main s390x apport-core-dump-handler all 2.28.1-0ubuntu1 [16.8 kB] 177s Get:4 http://ftpmaster.internal/ubuntu noble/main s390x apport all 2.28.1-0ubuntu1 [83.5 kB] 177s Get:5 http://ftpmaster.internal/ubuntu noble/main s390x libkeyutils1 s390x 1.6.3-3build1 [9556 B] 177s Get:6 http://ftpmaster.internal/ubuntu noble/main s390x netcat-openbsd s390x 1.226-1ubuntu2 [44.0 kB] 177s Get:7 http://ftpmaster.internal/ubuntu noble/main s390x libnuma1 s390x 2.0.18-1build1 [25.1 kB] 177s Get:8 http://ftpmaster.internal/ubuntu noble/main s390x man-db s390x 2.12.0-4build2 [1253 kB] 178s Get:9 http://ftpmaster.internal/ubuntu noble/main s390x make s390x 4.3-4.1build2 [196 kB] 178s Get:10 http://ftpmaster.internal/ubuntu noble/main s390x numactl s390x 2.0.18-1build1 [40.0 kB] 178s Preconfiguring packages ... 179s Fetched 1783 kB in 2s (1095 kB/s) 179s (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 ... 78323 files and directories currently installed.) 179s Preparing to unpack .../0-python3-problem-report_2.28.1-0ubuntu1_all.deb ... 179s Unpacking python3-problem-report (2.28.1-0ubuntu1) over (2.28.0-0ubuntu1) ... 179s Preparing to unpack .../1-python3-apport_2.28.1-0ubuntu1_all.deb ... 179s Unpacking python3-apport (2.28.1-0ubuntu1) over (2.28.0-0ubuntu1) ... 179s Preparing to unpack .../2-apport-core-dump-handler_2.28.1-0ubuntu1_all.deb ... 179s Unpacking apport-core-dump-handler (2.28.1-0ubuntu1) over (2.28.0-0ubuntu1) ... 179s Preparing to unpack .../3-apport_2.28.1-0ubuntu1_all.deb ... 179s Unpacking apport (2.28.1-0ubuntu1) over (2.28.0-0ubuntu1) ... 179s Preparing to unpack .../4-libkeyutils1_1.6.3-3build1_s390x.deb ... 179s Unpacking libkeyutils1:s390x (1.6.3-3build1) over (1.6.3-3) ... 179s Preparing to unpack .../5-netcat-openbsd_1.226-1ubuntu2_s390x.deb ... 179s Unpacking netcat-openbsd (1.226-1ubuntu2) over (1.226-1ubuntu1) ... 179s Preparing to unpack .../6-libnuma1_2.0.18-1build1_s390x.deb ... 179s Unpacking libnuma1:s390x (2.0.18-1build1) over (2.0.18-1) ... 179s Preparing to unpack .../7-man-db_2.12.0-4build2_s390x.deb ... 179s Unpacking man-db (2.12.0-4build2) over (2.12.0-4build1) ... 179s Preparing to unpack .../8-make_4.3-4.1build2_s390x.deb ... 179s Unpacking make (4.3-4.1build2) over (4.3-4.1build1) ... 179s Preparing to unpack .../9-numactl_2.0.18-1build1_s390x.deb ... 179s Unpacking numactl (2.0.18-1build1) over (2.0.18-1) ... 179s Setting up libkeyutils1:s390x (1.6.3-3build1) ... 179s Setting up python3-problem-report (2.28.1-0ubuntu1) ... 179s Setting up netcat-openbsd (1.226-1ubuntu2) ... 179s Setting up man-db (2.12.0-4build2) ... 179s Updating database of manual pages ... 181s man-db.service is a disabled or a static unit not running, not starting it. 181s Setting up python3-apport (2.28.1-0ubuntu1) ... 181s Setting up make (4.3-4.1build2) ... 181s Setting up libnuma1:s390x (2.0.18-1build1) ... 181s Setting up numactl (2.0.18-1build1) ... 181s Setting up apport-core-dump-handler (2.28.1-0ubuntu1) ... 182s Setting up apport (2.28.1-0ubuntu1) ... 182s Installing new version of config file /etc/apport/crashdb.conf ... 183s apport-autoreport.service is a disabled or a static unit not running, not starting it. 183s Processing triggers for libc-bin (2.39-0ubuntu8) ... 183s Reading package lists... 184s Building dependency tree... 184s Reading state information... 184s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 184s Hit:1 http://ftpmaster.internal/ubuntu noble InRelease 184s Hit:2 http://ftpmaster.internal/ubuntu noble-updates InRelease 184s Hit:3 http://ftpmaster.internal/ubuntu noble-security InRelease 185s Hit:4 http://ftpmaster.internal/ubuntu noble-proposed InRelease 186s Reading package lists... 186s Reading package lists... 186s Building dependency tree... 186s Reading state information... 186s Calculating upgrade... 186s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 186s Reading package lists... 187s Building dependency tree... 187s Reading state information... 187s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 187s autopkgtest [00:37:52]: rebooting testbed after setup commands that affected boot 224s autopkgtest [00:38:29]: testbed running kernel: Linux 6.8.0-22-generic #22-Ubuntu SMP Thu Apr 4 21:54:17 UTC 2024 227s autopkgtest [00:38:32]: @@@@@@@@@@@@@@@@@@@@ apt-source cpl-plugin-muse 231s Get:1 http://ftpmaster.internal/ubuntu noble/universe cpl-plugin-muse 2.8.7+dfsg-3 (dsc) [2420 B] 231s Get:2 http://ftpmaster.internal/ubuntu noble/universe cpl-plugin-muse 2.8.7+dfsg-3 (tar) [1586 kB] 231s Get:3 http://ftpmaster.internal/ubuntu noble/universe cpl-plugin-muse 2.8.7+dfsg-3 (diff) [14.6 kB] 231s gpgv: Signature made Tue Aug 16 06:12:08 2022 UTC 231s gpgv: using RSA key BAFC6C85F7CB143FEEB6FB157115AFD07710DCF7 231s gpgv: Can't check signature: No public key 231s dpkg-source: warning: cannot verify inline signature for ./cpl-plugin-muse_2.8.7+dfsg-3.dsc: no acceptable signature found 232s autopkgtest [00:38:37]: testing package cpl-plugin-muse version 2.8.7+dfsg-3 232s autopkgtest [00:38:37]: build not needed 233s autopkgtest [00:38:38]: test test-recipe.py: preparing testbed 235s Reading package lists... 235s Building dependency tree... 235s Reading state information... 235s Starting pkgProblemResolver with broken count: 0 235s Starting 2 pkgProblemResolver with broken count: 0 235s Done 235s The following additional packages will be installed: 235s cpl-plugin-muse libblas3 libcext0 libcfitsio10t64 libcplcore26 libcpldfs26 235s libcpldrs26 libcplui26 liberfa1 libfftw3-double3 libfftw3-single3 235s libgfortran5 libgomp1 libgsl27 libgslcblas0 libjs-jquery 235s libjs-jquery-hotkeys libjs-jquery-isonscreen libjs-jquery-metadata 235s libjs-jquery-tablesorter libjs-jquery-throttle-debounce libjs-sphinxdoc 235s libjs-underscore liblapack3 libwcs8 python3-astropy 235s python3-astropy-iers-data python3-coverage python3-cpl python3-dateutil 235s python3-erfa python3-hypothesis python3-iniconfig python3-numpy 235s python3-packaging python3-pluggy python3-ply python3-pytest 235s python3-pytest-arraydiff python3-pytest-astropy 235s python3-pytest-astropy-header python3-pytest-cov python3-pytest-doctestplus 235s python3-pytest-filter-subpackage python3-pytest-mock 235s python3-pytest-remotedata python3-sortedcontainers 235s Suggested packages: 235s cpl-plugin-muse-calib cpl-plugin-muse-doc libfftw3-bin libfftw3-dev 235s gsl-ref-psdoc | gsl-doc-pdf | gsl-doc-info | gsl-ref-html libxml2-utils 235s python-astropy-doc python3-astropy-affiliated python3-bs4 python3-h5py 235s python3-matplotlib python3-pandas python-coverage-doc gdb 235s python-hypothesis-doc gcc gfortran python3-dev python-ply-doc 235s python-pytest-mock-doc python-sortedcontainers-doc 235s Recommended packages: 235s javascript-common libjs-jquery-datatables python3-scipy python3-click 236s The following NEW packages will be installed: 236s autopkgtest-satdep cpl-plugin-muse libblas3 libcext0 libcfitsio10t64 236s libcplcore26 libcpldfs26 libcpldrs26 libcplui26 liberfa1 libfftw3-double3 236s libfftw3-single3 libgfortran5 libgomp1 libgsl27 libgslcblas0 libjs-jquery 236s libjs-jquery-hotkeys libjs-jquery-isonscreen libjs-jquery-metadata 236s libjs-jquery-tablesorter libjs-jquery-throttle-debounce libjs-sphinxdoc 236s libjs-underscore liblapack3 libwcs8 python3-astropy 236s python3-astropy-iers-data python3-coverage python3-cpl python3-dateutil 236s python3-erfa python3-hypothesis python3-iniconfig python3-numpy 236s python3-packaging python3-pluggy python3-ply python3-pytest 236s python3-pytest-arraydiff python3-pytest-astropy 236s python3-pytest-astropy-header python3-pytest-cov python3-pytest-doctestplus 236s python3-pytest-filter-subpackage python3-pytest-mock 236s python3-pytest-remotedata python3-sortedcontainers 236s 0 upgraded, 48 newly installed, 0 to remove and 0 not upgraded. 236s Need to get 20.8 MB/20.8 MB of archives. 236s After this operation, 89.0 MB of additional disk space will be used. 236s Get:1 /tmp/autopkgtest.93Zlzg/1-autopkgtest-satdep.deb autopkgtest-satdep s390x 0 [724 B] 236s Get:2 http://ftpmaster.internal/ubuntu noble/main s390x libjs-jquery all 3.6.1+dfsg+~3.5.14-1 [328 kB] 236s Get:3 http://ftpmaster.internal/ubuntu noble/universe s390x libjs-jquery-hotkeys all 0~20130707+git2d51e3a9+dfsg-2ubuntu2 [11.5 kB] 236s Get:4 http://ftpmaster.internal/ubuntu noble/universe s390x libcext0 s390x 7.3.2+ds-1build3 [33.9 kB] 236s Get:5 http://ftpmaster.internal/ubuntu noble/universe s390x libcfitsio10t64 s390x 4.3.1-1.1build2 [609 kB] 238s Get:6 http://ftpmaster.internal/ubuntu noble/main s390x libgomp1 s390x 14-20240412-0ubuntu1 [151 kB] 238s Get:7 http://ftpmaster.internal/ubuntu noble/main s390x libfftw3-double3 s390x 3.3.10-1ubuntu3 [512 kB] 239s Get:8 http://ftpmaster.internal/ubuntu noble/main s390x libfftw3-single3 s390x 3.3.10-1ubuntu3 [481 kB] 240s Get:9 http://ftpmaster.internal/ubuntu noble/universe s390x libcplcore26 s390x 7.3.2+ds-1build3 [600 kB] 240s Get:10 http://ftpmaster.internal/ubuntu noble/universe s390x libcplui26 s390x 7.3.2+ds-1build3 [37.9 kB] 240s Get:11 http://ftpmaster.internal/ubuntu noble/universe s390x libcpldfs26 s390x 7.3.2+ds-1build3 [41.8 kB] 240s Get:12 http://ftpmaster.internal/ubuntu noble/universe s390x libwcs8 s390x 8.2.2+ds-3build2 [289 kB] 241s Get:13 http://ftpmaster.internal/ubuntu noble/universe s390x libcpldrs26 s390x 7.3.2+ds-1build3 [73.4 kB] 241s Get:14 http://ftpmaster.internal/ubuntu noble-proposed/universe s390x libgslcblas0 s390x 2.7.1+dfsg-6ubuntu2 [150 kB] 241s Get:15 http://ftpmaster.internal/ubuntu noble-proposed/universe s390x libgsl27 s390x 2.7.1+dfsg-6ubuntu2 [1084 kB] 242s Get:16 http://ftpmaster.internal/ubuntu noble/universe s390x cpl-plugin-muse s390x 2.8.7+dfsg-3 [512 kB] 243s Get:17 http://ftpmaster.internal/ubuntu noble/main s390x libblas3 s390x 3.12.0-3build1 [245 kB] 243s Get:18 http://ftpmaster.internal/ubuntu noble/main s390x libgfortran5 s390x 14-20240412-0ubuntu1 [600 kB] 243s Get:19 http://ftpmaster.internal/ubuntu noble/universe s390x libjs-jquery-metadata all 12-4 [6582 B] 243s Get:20 http://ftpmaster.internal/ubuntu noble/universe s390x libjs-jquery-tablesorter all 1:2.31.3+dfsg1-3 [193 kB] 244s Get:21 http://ftpmaster.internal/ubuntu noble/universe s390x libjs-jquery-throttle-debounce all 1.1+dfsg.1-2 [12.5 kB] 244s Get:22 http://ftpmaster.internal/ubuntu noble/main s390x libjs-underscore all 1.13.4~dfsg+~1.11.4-3 [118 kB] 244s Get:23 http://ftpmaster.internal/ubuntu noble/main s390x libjs-sphinxdoc all 7.2.6-6 [149 kB] 244s Get:24 http://ftpmaster.internal/ubuntu noble/main s390x liblapack3 s390x 3.12.0-3build1 [2976 kB] 246s Get:25 http://ftpmaster.internal/ubuntu noble/universe s390x python3-iniconfig all 1.1.1-2 [6024 B] 246s Get:26 http://ftpmaster.internal/ubuntu noble/main s390x python3-packaging all 24.0-1 [41.1 kB] 246s Get:27 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pluggy all 1.4.0-1 [20.4 kB] 246s Get:28 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pytest all 7.4.4-1 [305 kB] 246s Get:29 http://ftpmaster.internal/ubuntu noble/main s390x python3-dateutil all 2.8.2-3ubuntu1 [79.4 kB] 246s Get:30 http://ftpmaster.internal/ubuntu noble/main s390x python3-sortedcontainers all 2.4.0-2 [27.6 kB] 246s Get:31 http://ftpmaster.internal/ubuntu noble/universe s390x python3-hypothesis all 6.98.15-1 [311 kB] 246s Get:32 http://ftpmaster.internal/ubuntu noble/main s390x python3-numpy s390x 1:1.26.4+ds-6ubuntu1 [4119 kB] 250s Get:33 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pytest-arraydiff all 0.6.1-2 [10.2 kB] 250s Get:34 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pytest-astropy-header all 0.2.2-1 [8190 B] 250s Get:35 http://ftpmaster.internal/ubuntu noble/universe s390x python3-coverage s390x 7.4.4+dfsg1-0ubuntu2 [147 kB] 251s Get:36 http://ftpmaster.internal/ubuntu noble/universe s390x libjs-jquery-isonscreen all 1.2.0-1.1 [3244 B] 251s Get:37 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pytest-cov all 4.1.0-1 [21.5 kB] 251s Get:38 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pytest-doctestplus all 1.2.0-1 [23.1 kB] 251s Get:39 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pytest-filter-subpackage all 0.2.0-1 [6094 B] 251s Get:40 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pytest-mock all 3.12.0-1.1 [11.3 kB] 251s Get:41 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pytest-remotedata all 0.4.1-1 [8650 B] 251s Get:42 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pytest-astropy all 0.11.0-1 [5902 B] 251s Get:43 http://ftpmaster.internal/ubuntu noble/main s390x python3-ply all 3.11-6 [46.5 kB] 251s Get:44 http://ftpmaster.internal/ubuntu noble/universe s390x python3-astropy-iers-data all 0.2024.01.01.00.33.39-1 [2046 kB] 253s Get:45 http://ftpmaster.internal/ubuntu noble/universe s390x liberfa1 s390x 2.0.1-1 [136 kB] 253s Get:46 http://ftpmaster.internal/ubuntu noble/universe s390x python3-erfa s390x 2.0.1.1+ds-3 [314 kB] 254s Get:47 http://ftpmaster.internal/ubuntu noble/universe s390x python3-astropy s390x 6.0.0-1ubuntu2 [3859 kB] 257s Get:48 http://ftpmaster.internal/ubuntu noble/universe s390x python3-cpl s390x 0.7.4-2build10 [35.1 kB] 258s Fetched 20.8 MB in 22s (957 kB/s) 258s Selecting previously unselected package libjs-jquery. 258s (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 ... 78322 files and directories currently installed.) 258s Preparing to unpack .../00-libjs-jquery_3.6.1+dfsg+~3.5.14-1_all.deb ... 258s Unpacking libjs-jquery (3.6.1+dfsg+~3.5.14-1) ... 258s Selecting previously unselected package libjs-jquery-hotkeys. 258s Preparing to unpack .../01-libjs-jquery-hotkeys_0~20130707+git2d51e3a9+dfsg-2ubuntu2_all.deb ... 258s Unpacking libjs-jquery-hotkeys (0~20130707+git2d51e3a9+dfsg-2ubuntu2) ... 258s Selecting previously unselected package libcext0:s390x. 258s Preparing to unpack .../02-libcext0_7.3.2+ds-1build3_s390x.deb ... 258s Unpacking libcext0:s390x (7.3.2+ds-1build3) ... 258s Selecting previously unselected package libcfitsio10t64:s390x. 258s Preparing to unpack .../03-libcfitsio10t64_4.3.1-1.1build2_s390x.deb ... 258s Unpacking libcfitsio10t64:s390x (4.3.1-1.1build2) ... 258s Selecting previously unselected package libgomp1:s390x. 258s Preparing to unpack .../04-libgomp1_14-20240412-0ubuntu1_s390x.deb ... 258s Unpacking libgomp1:s390x (14-20240412-0ubuntu1) ... 258s Selecting previously unselected package libfftw3-double3:s390x. 258s Preparing to unpack .../05-libfftw3-double3_3.3.10-1ubuntu3_s390x.deb ... 258s Unpacking libfftw3-double3:s390x (3.3.10-1ubuntu3) ... 258s Selecting previously unselected package libfftw3-single3:s390x. 258s Preparing to unpack .../06-libfftw3-single3_3.3.10-1ubuntu3_s390x.deb ... 258s Unpacking libfftw3-single3:s390x (3.3.10-1ubuntu3) ... 258s Selecting previously unselected package libcplcore26:s390x. 258s Preparing to unpack .../07-libcplcore26_7.3.2+ds-1build3_s390x.deb ... 258s Unpacking libcplcore26:s390x (7.3.2+ds-1build3) ... 258s Selecting previously unselected package libcplui26:s390x. 258s Preparing to unpack .../08-libcplui26_7.3.2+ds-1build3_s390x.deb ... 258s Unpacking libcplui26:s390x (7.3.2+ds-1build3) ... 258s Selecting previously unselected package libcpldfs26:s390x. 258s Preparing to unpack .../09-libcpldfs26_7.3.2+ds-1build3_s390x.deb ... 258s Unpacking libcpldfs26:s390x (7.3.2+ds-1build3) ... 258s Selecting previously unselected package libwcs8:s390x. 258s Preparing to unpack .../10-libwcs8_8.2.2+ds-3build2_s390x.deb ... 258s Unpacking libwcs8:s390x (8.2.2+ds-3build2) ... 258s Selecting previously unselected package libcpldrs26:s390x. 258s Preparing to unpack .../11-libcpldrs26_7.3.2+ds-1build3_s390x.deb ... 258s Unpacking libcpldrs26:s390x (7.3.2+ds-1build3) ... 258s Selecting previously unselected package libgslcblas0:s390x. 258s Preparing to unpack .../12-libgslcblas0_2.7.1+dfsg-6ubuntu2_s390x.deb ... 258s Unpacking libgslcblas0:s390x (2.7.1+dfsg-6ubuntu2) ... 258s Selecting previously unselected package libgsl27:s390x. 258s Preparing to unpack .../13-libgsl27_2.7.1+dfsg-6ubuntu2_s390x.deb ... 258s Unpacking libgsl27:s390x (2.7.1+dfsg-6ubuntu2) ... 258s Selecting previously unselected package cpl-plugin-muse:s390x. 258s Preparing to unpack .../14-cpl-plugin-muse_2.8.7+dfsg-3_s390x.deb ... 258s Unpacking cpl-plugin-muse:s390x (2.8.7+dfsg-3) ... 258s Selecting previously unselected package libblas3:s390x. 258s Preparing to unpack .../15-libblas3_3.12.0-3build1_s390x.deb ... 258s Unpacking libblas3:s390x (3.12.0-3build1) ... 258s Selecting previously unselected package libgfortran5:s390x. 258s Preparing to unpack .../16-libgfortran5_14-20240412-0ubuntu1_s390x.deb ... 258s Unpacking libgfortran5:s390x (14-20240412-0ubuntu1) ... 258s Selecting previously unselected package 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(0.7.4-2build10) ... 269s Setting up autopkgtest-satdep (0) ... 269s Processing triggers for man-db (2.12.0-4build2) ... 270s Processing triggers for libc-bin (2.39-0ubuntu8) ... 273s (Reading database ... 82210 files and directories currently installed.) 273s Removing autopkgtest-satdep (0) ... 274s autopkgtest [00:39:19]: test test-recipe.py: [----------------------- 274s Recipe muse_geometry: 274s version 2.8.7 274s Parameters: {'ifu1': 1, 'ifu2': 24, 'sigma': 2.2, 'centroid': 'gaussian', 'smooth': 1.5, 'lambdamin': 6800.0, 'lambdamax': 7200.0} 274s Docstring: Compute relative location of the slices within the field of view and 274s measure the instrumental PSF on the detectors. 274s 274s Processing first works separately on each IFU of the raw input data 274s (in parallel): it trims the raw data and records the overscan 274s statistics, subtracts the bias and converts them from adu to count. 274s Optionally, the dark can be subtracted and the data can be divided by 274s the flat-field. The data of all input mask exposures is then averaged. 274s The averaged image together with the trace table and wavelength 274s calibration as well as the line catalog are used to detect spots. The 274s detection windows are used to measure the spots on all images of the 274s sequence, the result is saved, with information on the measured PSF, 274s in the spots tables. Then properties of all slices are computed, first 274s separately on each IFU to determine the peak position of the mask for 274s each slice and its angle, subsequently the width and horizontal 274s position. Then, the result of all IFUs is analyzed together to produce 274s a refined horizontal position, applying global shifts to each IFU as 274s needed. The vertical position is then determined using the known slice 274s ordering on the sky; the relative peak positions are put into 274s sequence, taking into account the vertical offsets of the pinholes in 274s the mask. The table is then cleaned up from intermediate debug data. 274s If the --smooth parameter is set to a positive value, it is used to do 274s a sigma-clipped smoothing within each slicer stack, for a more regular 274s appearance of the output table. The table is then saved. As a last 274s optional step, additional raw input data is reduced using the newly 274s geometry to produce an image of the field of view. If these exposures 274s contain smooth features, they can be used as a visual check of the 274s quality of the geometrical calibration. 274s 274s Parameters: 274s ifu1: First IFU to analyze. (int; default: 1) 274s ifu2: Last IFU to analyze. (int; default: 24) 274s sigma: Sigma detection level for spot detection, in terms of 274s median deviation above the median. (float; default: 2.2) 274s centroid: Type of centroiding and FWHM determination to use for all 274s spot measurements: simple barycenter method or using a 274s Gaussian fit. (str; default: 'gaussian') 274s smooth: Use this sigma-level cut for smoothing of the output table 274s within each slicer stack. Set to non-positive value to 274s deactivate smoothing. (float; default: 1.5) 274s lambdamin: When passing any MASK_CHECK frames in the input, use this 274s lower wavelength cut before reconstructing the image. 274s (float; default: 6800.0) 274s lambdamax: When passing any MASK_CHECK frames in the input, use this 274s upper wavelength cut before reconstructing the image. 274s (float; default: 7200.0) 274s 274s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 274s 'TRACE_TABLE', 'WAVECAL_TABLE', 'LINE_CATALOG', 274s 'BADPIX_TABLE', 'MASK_CHECK'] 274s 274s Raw and product frames: 274s MASK --> ['MASK_REDUCED', 'MASK_COMBINED', 'SPOTS_TABLE', 274s 'GEOMETRY_UNSMOOTHED', 'GEOMETRY_TABLE', 'GEOMETRY_CUBE'] 274s Author: Peter Weilbacher 274s 274s 274s Recipe muse_illum: 274s version 2.8.7 274s Parameters: {} 274s Docstring: Dummy recipe to convert a raw illumination flat field into a DFS 274s product 274s 274s The recipe copies the data of an illumination flat-field unmodified to 274s the output file. However it alters the header data such that the 274s result is a DFS compliant product file, which can be used in the on- 274s line pipeline environment to correct the illumination of twilight 274s and/or science observations. This recipe has no use in any environment 274s other than the on-line pipeline environment! 274s 274s No parameters 274s Calibration frames: [] 274s 274s Raw and product frames: 274s ILLUMFLAT --> ['ILLUM'] 274s Author: Ralf Palsa 274s 274s 274s Recipe muse_bias: 274s version 2.8.7 274s 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} 274s Docstring: Combine several separate bias images into one master bias file. 274s 274s This recipe combines several separate bias images into one master bias 274s file. The master bias contains the combined pixel values, in adu, of 274s the raw bias exposures, with respect to the image combination method 274s used. Processing trims the raw data and records the overscan 274s statistics, corrects the data levels using the overscan (if overscan 274s is not "none") and combines the exposures using input parameters. The 274s read-out noise is computed for each quadrant of the raw input images 274s and stored as QC parameter. The variance extension is filled with an 274s initial value accordingly, before image combination. Further QC 274s statistics are computed on the output master bias. Additionally, bad 274s columns are searched for and marked in the data quality extension. 274s 274s Parameters: 274s nifu: IFU to handle. If set to 0, all IFUs are processed 274s serially. If set to -1, all IFUs are processed in 274s parallel. (int; default: 0) 274s overscan: If this is "none", stop when detecting discrepant 274s overscan levels (see ovscsigma), for "offset" it 274s assumes that the mean overscan level represents the 274s real offset in the bias levels of the exposures 274s involved, and adjusts the data accordingly; for 274s "vpoly", a polynomial is fit to the vertical overscan 274s and subtracted from the whole quadrant. (str; default: 274s 'vpoly') 274s ovscreject: This influences how values are rejected when computing 274s overscan statistics. Either no rejection at all 274s ("none"), rejection using the DCR algorithm ("dcr"), 274s or rejection using an iterative constant fit ("fit"). 274s (str; default: 'dcr') 274s ovscsigma: If the deviation of mean overscan levels between a raw 274s input image and the reference image is higher than 274s |ovscsigma x stdev|, stop the processing. If 274s overscan="vpoly", this is used as sigma rejection 274s level for the iterative polynomial fit (the level 274s comparison is then done afterwards with |100 x stdev| 274s to guard against incompatible settings). Has no effect 274s for overscan="offset". (float; default: 30.0) 274s ovscignore: The number of pixels of the overscan adjacent to the 274s data section of the CCD that are ignored when 274s computing statistics or fits. (int; default: 3) 274s combine: Type of image combination to use. (str; default: 274s 'sigclip') 274s nlow: Number of minimum pixels to reject with minmax. (int; 274s default: 1) 274s nhigh: Number of maximum pixels to reject with minmax. (int; 274s default: 1) 274s nkeep: Number of pixels to keep with minmax. (int; default: 274s 1) 274s lsigma: Low sigma for pixel rejection with sigclip. (float; 274s default: 3.0) 274s hsigma: High sigma for pixel rejection with sigclip. (float; 274s default: 3.0) 274s losigmabadpix: Low sigma to find dark columns in the combined bias 274s (float; default: 30.0) 274s hisigmabadpix: High sigma to find bright columns in the combined bias 274s (float; default: 3.0) 274s merge: Merge output products from different IFUs into a 274s common file. (bool; default: False) 274s 274s Calibration frames: ['BADPIX_TABLE'] 274s 274s Raw and product frames: 274s BIAS --> ['MASTER_BIAS'] 274s Author: Peter Weilbacher 274s 274s 274s Recipe muse_scipost_correct_dar: 274s version 2.8.7 274s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'lambdaref': 7000.0, 'darcheck': 'none'} 274s Docstring: Apply DAR correction for MUSE pixel tables. 274s 274s Correct the coordinates in the pixel table by differential atmospheric 274s refraction. This is a task separated from muse_scipost. 274s 274s Parameters: 274s lambdamin: Cut off the data below this wavelength after loading the 274s pixel table(s). (float; default: 4000.0) 274s lambdamax: Cut off the data above this wavelength after loading the 274s pixel table(s). (float; default: 10000.0) 274s lambdaref: Reference wavelength used for correction of differential 274s atmospheric refraction. The R-band (peak wavelength ~7000 274s Angstrom) that is usually used for guiding, is close to 274s the central wavelength of MUSE, so a value of 7000.0 274s Angstrom should be used if nothing else is known. A value 274s less than zero switches DAR correction off. (float; 274s default: 7000.0) 274s darcheck: Carry out a check of the theoretical DAR correction using 274s source centroiding. If "correct" it will also apply an 274s empirical correction. (str; default: 'none') 274s 274s Calibration frames: [] 274s 274s Raw and product frames: 274s PIXTABLE_OBJECT --> ['PIXTABLE_OBJECT'] 274s Author: Ole Streicher 274s 274s 274s Recipe muse_lsf: 274s version 2.8.7 274s 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'} 274s Docstring: Compute the LSF 274s 274s Compute the slice and wavelength dependent LSF from a lines spectrum 274s (ARC lamp). 274s 274s Parameters: 274s nifu: IFU to handle. If set to 0, all IFUs are 274s processed serially. If set to -1, all IFUs are 274s processed in parallel. (int; default: 0) 274s overscan: If this is "none", stop when detecting 274s discrepant overscan levels (see ovscsigma), 274s for "offset" it assumes that the mean overscan 274s level represents the real offset in the bias 274s levels of the exposures involved, and adjusts 274s the data accordingly; for "vpoly", a 274s polynomial is fit to the vertical overscan and 274s subtracted from the whole quadrant. (str; 274s default: 'vpoly') 274s ovscreject: This influences how values are rejected when 274s computing overscan statistics. Either no 274s rejection at all ("none"), rejection using the 274s DCR algorithm ("dcr"), or rejection using an 274s iterative constant fit ("fit"). (str; default: 274s 'dcr') 274s ovscsigma: If the deviation of mean overscan levels 274s between a raw input image and the reference 274s image is higher than |ovscsigma x stdev|, stop 274s the processing. If overscan="vpoly", this is 274s used as sigma rejection level for the 274s iterative polynomial fit (the level comparison 274s is then done afterwards with |100 x stdev| to 274s guard against incompatible settings). Has no 274s effect for overscan="offset". (float; default: 274s 30.0) 274s ovscignore: The number of pixels of the overscan adjacent 274s to the data section of the CCD that are 274s ignored when computing statistics or fits. 274s (int; default: 3) 274s save_subtracted: Save the pixel table after the LSF 274s subtraction. (bool; default: False) 274s line_quality: Minimal quality flag in line catalog for 274s selection (int; default: 3) 274s lsf_range: Wavelength window (half size) around each line 274s to estimate LSF (float; default: 7.5) 274s lsf_size: Image size in LSF direction (int; default: 274s 150) 274s lambda_size: Image size in line wavelength direction (int; 274s default: 30) 274s lsf_regression_window: Size of the regression window in LSF direction 274s (float; default: 0.7) 274s merge: Merge output products from different IFUs into 274s a common file. (bool; default: False) 274s combine: Type of lampwise image combination to use. 274s (str; default: 'sigclip') 274s method: LSF generation method. Depending on this 274s value, either an interpolated LSF cube is 274s created, or a table with the parameters of a 274s hermitean gaussian. (str; default: 274s 'interpolate') 274s 274s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 274s 'TRACE_TABLE', 'WAVECAL_TABLE', 'BADPIX_TABLE', 274s 'LINE_CATALOG'] 274s 274s Raw and product frames: 274s ARC --> ['LSF_PROFILE', 'PIXTABLE_SUBTRACTED'] 274s ARC_LSF --> ['LSF_PROFILE', 'PIXTABLE_SUBTRACTED'] 274s Author: Ole Streicher 274s 274s 274s Recipe muse_scipost_calibrate_flux: 274s version 2.8.7 274s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0} 274s Docstring: Calibrate flux for MUSE pixel tables. 274s 274s Replace the intensity in the MUSE pixel tables by the absolute flux. 274s This is a task separated from muse_scipost. 274s 274s Parameters: 274s lambdamin: Cut off the data below this wavelength after loading the 274s pixel table(s). (float; default: 4000.0) 274s lambdamax: Cut off the data above this wavelength after loading the 274s pixel table(s). (float; default: 10000.0) 274s 274s Calibration frames: ['EXTINCT_TABLE', 'STD_RESPONSE', 'STD_TELLURIC'] 274s 274s Raw and product frames: 274s PIXTABLE_OBJECT --> ['PIXTABLE_OBJECT'] 274s Author: Ole Streicher 274s 274s 274s Recipe muse_standard: 274s version 2.8.7 274s Parameters: {'profile': 'auto', 'select': 'distance', 'smooth': 'ppoly', 'lambdamin': 4000.0, 'lambdamax': 10000.0, 'lambdaref': 7000.0, 'darcheck': 'none', 'filter': 'white'} 274s Docstring: Create a flux response curve from a standard star exposure. 274s 274s Merge pixel tables from all IFUs and correct for differential 274s atmospheric refraction, when necessary. To derive the flux response 274s curve, integrate the flux of all objects detected within the field of 274s view using the given profile. Select one object as the standard star 274s (either the brightest or the one nearest one, depending on --select) 274s and compare its measured fluxes to tabulated fluxes to derive the 274s sensitivity over wavelength. Postprocess this sensitivity curve to 274s mark wavelength ranges affected by telluric absorption. Interpolate 274s over the telluric regions and derive a telluric correction spectrum 274s for them. The final response curve is then linearly extrapolated to 274s the largest possible MUSE wavelength range and smoothed (with the 274s method given by --smooth). The derivation of the telluric correction 274s spectrum assumes that the star has a smooth spectrum within the 274s telluric regions. If there are more than one exposure given in the 274s input data, the derivation of the flux response and telluric 274s corrections are done separately for each exposure. For each exposure, 274s an image containing the extracted stellar spectra and the datacube 274s used for flux integration are saved, together with collapsed images 274s for each given filter. In MUSE's WFM data (both AO and non-AO), the 274s Moffat profile is a good approximation of the actual PSF. Using the 274s smoothed profile ("smoffat") helps to increase the S/N and in most 274s cases removes systematics. In NFM, however, the profile is a 274s combination of a wide PSF plus the central AO-corrected peak, which 274s cannot be fit well by an analytical profile. In this case the circular 274s aperture is the best way to extract the flux. Using --profile="auto" 274s (the default) selects these options to give the best flux extraction 274s for most cases. 274s 274s Parameters: 274s profile: Type of flux integration to use. "gaussian", "moffat", and 274s "smoffat" use 2D profile fitting, "circle" and "square" 274s are non-optimal aperture flux integrators. "smoffat" uses 274s smoothing of the Moffat parameters from an initial fit, to 274s derive physically meaningful wavelength- dependent 274s behavior. "auto" selects the smoothed Moffat profile for 274s WFM data and circular flux integration for NFM. (str; 274s default: 'auto') 274s select: How to select the star for flux integration, "flux" uses 274s the brightest star in the field, "distance" uses the 274s detection nearest to the approximate coordinates of the 274s reference source. (str; default: 'distance') 274s smooth: How to smooth the response curve before writing it to 274s disk. "none" does not do any kind of smoothing (such a 274s response curve is only useful, if smoothed externally; 274s "median" does a median-filter of 15 Angstrom half-width; 274s "ppoly" fits piecewise cubic polynomials (each one across 274s 2x150 Angstrom width) postprocessed by a sliding average 274s filter of 15 Angstrom half-width. (str; default: 'ppoly') 274s lambdamin: Cut off the data below this wavelength after loading the 274s pixel table(s). (float; default: 4000.0) 274s lambdamax: Cut off the data above this wavelength after loading the 274s pixel table(s). (float; default: 10000.0) 274s lambdaref: Reference wavelength used for correction of differential 274s atmospheric refraction. The R-band (peak wavelength ~7000 274s Angstrom) that is usually used for guiding, is close to 274s the central wavelength of MUSE, so a value of 7000.0 274s Angstrom should be used if nothing else is known. A value 274s less than zero switches DAR correction off. (float; 274s default: 7000.0) 274s darcheck: Carry out a check of the theoretical DAR correction using 274s source centroiding. If "correct" it will also apply an 274s empirical correction. (str; default: 'none') 274s filter: The filter name(s) to be used for the output field-of-view 274s image. Each name has to correspond to an EXTNAME in an 274s extension of the FILTER_LIST file. If an unsupported 274s filter name is given, creation of the respective image is 274s omitted. If multiple filter names are given, they have to 274s be comma separated. If the zeropoint QC parameters are 274s wanted, make sure to add "Johnson_V,Cousins_R,Cousins_I". 274s (str; default: 'white') 274s 274s Calibration frames: ['EXTINCT_TABLE', 'STD_FLUX_TABLE', 274s 'TELLURIC_REGIONS', 'FILTER_LIST'] 274s 274s Raw and product frames: 274s PIXTABLE_STD --> ['DATACUBE_STD', 'STD_FLUXES', 'STD_RESPONSE', 274s 'STD_TELLURIC'] 274s Author: Peter Weilbacher 274s 274s 274s Recipe muse_dark: 274s version 2.8.7 274s 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} 274s Docstring: Combine several separate dark images into one master dark file and 274s locate hot pixels. 274s 274s This recipe combines several separate dark images into one master dark 274s file. The master dark contains the combined pixel values of the raw 274s dark exposures, with respect to the image combination method used and 274s normalization time specified. Processing trims the raw data and 274s records the overscan statistics, subtracts the bias (taking account of 274s the overscan, if --overscan is not "none") from each raw input image, 274s converts them from adu to count, scales them according to their 274s exposure time, and combines them using input parameters. Hot pixels 274s are then identified using image statistics and marked in the data 274s quality extension. The combined image is normalized to 1 hour exposure 274s time. QC statistics are computed on the output master dark. If 274s --model=true, a smooth polynomial model of the combined master dark is 274s computed, created from several individual 2D polynomials to describe 274s different features visible in MUSE dark frames. It is only advisable 274s to use this, if the master dark is the result of at least 50 274s individual long dark exposures. 274s 274s Parameters: 274s nifu: IFU to handle. If set to 0, all IFUs are processed 274s serially. If set to -1, all IFUs are processed in 274s parallel. (int; default: 0) 274s overscan: If this is "none", stop when detecting discrepant 274s overscan levels (see ovscsigma), for "offset" it assumes 274s that the mean overscan level represents the real offset 274s in the bias levels of the exposures involved, and adjusts 274s the data accordingly; for "vpoly", a polynomial is fit to 274s the vertical overscan and subtracted from the whole 274s quadrant. (str; default: 'vpoly') 274s ovscreject: This influences how values are rejected when computing 274s overscan statistics. Either no rejection at all ("none"), 274s rejection using the DCR algorithm ("dcr"), or rejection 274s using an iterative constant fit ("fit"). (str; default: 274s 'dcr') 274s ovscsigma: If the deviation of mean overscan levels between a raw 274s input image and the reference image is higher than 274s |ovscsigma x stdev|, stop the processing. If 274s overscan="vpoly", this is used as sigma rejection level 274s for the iterative polynomial fit (the level comparison is 274s then done afterwards with |100 x stdev| to guard against 274s incompatible settings). Has no effect for 274s overscan="offset". (float; default: 30.0) 274s ovscignore: The number of pixels of the overscan adjacent to the data 274s section of the CCD that are ignored when computing 274s statistics or fits. (int; default: 3) 274s combine: Type of image combination to use. (str; default: 274s 'sigclip') 274s nlow: Number of minimum pixels to reject with minmax. (int; 274s default: 1) 274s nhigh: Number of maximum pixels to reject with minmax. (int; 274s default: 1) 274s nkeep: Number of pixels to keep with minmax. (int; default: 1) 274s lsigma: Low sigma for pixel rejection with sigclip. (float; 274s default: 3.0) 274s hsigma: High sigma for pixel rejection with sigclip. (float; 274s default: 3.0) 274s scale: Scale the individual images to a common exposure time 274s before combining them. (bool; default: True) 274s normalize: Normalize the master dark to this exposure time (in 274s seconds). To disable normalization, set this to a 274s negative value. (float; default: 3600.0) 274s hotsigma: Sigma level, in terms of median deviation above the 274s median dark level, above which a pixel is detected and 274s marked as 'hot'. (float; default: 5.0) 274s model: Model the master dark using a set of polynomials. (bool; 274s default: False) 274s merge: Merge output products from different IFUs into a common 274s file. (bool; default: False) 274s 274s Calibration frames: ['MASTER_BIAS', 'BADPIX_TABLE'] 274s 274s Raw and product frames: 274s DARK --> ['MASTER_DARK', 'MODEL_DARK'] 274s Author: Peter Weilbacher 274s 274s 274s Recipe muse_scipost_raman: 274s version 2.8.7 274s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'lambdaref': 7000.0, 'width': 20.0, 'crsigma': 15.0, 'fraction': 0.75, 'ignore': 0.05} 274s Docstring: Remove of 4GLSF Raman emission. 274s 274s This recipe removes the Raman scattered light of the 4GLSF system from 274s the exposure. It must be before the normal sky subtraction. 274s 274s Parameters: 274s lambdamin: Cut off the data below this wavelength after loading the 274s pixel table(s). (float; default: 4000.0) 274s lambdamax: Cut off the data above this wavelength after loading the 274s pixel table(s). (float; default: 10000.0) 274s lambdaref: Reference wavelength used for correction of differential 274s atmospheric refraction. The R-band (peak wavelength ~7000 274s Angstrom) that is usually used for guiding, is close to 274s the central wavelength of MUSE, so a value of 7000.0 274s Angstrom should be used if nothing else is known. A value 274s less than zero switches DAR correction off. (float; 274s default: 7000.0) 274s width: Wavelength range around Raman lines [Angstrom]. (float; 274s default: 20.0) 274s crsigma: Sigma level clipping for cube-based CR rejection (using 274s "median", see muse_scipost). It can be switched off, by 274s passing zero or a negative value. (float; default: 15.0) 274s fraction: Fraction of the image (without the ignored part) to be 274s considered as sky. If an input sky mask is provided, the 274s fraction is applied to the regions within the mask. If the 274s whole sky mask should be used, set this parameter to 1. 274s (float; default: 0.75) 274s ignore: Lowest fraction of the image to be ignored. If an input 274s sky mask is provided, the fraction is applied to the 274s regions within the mask. If the whole sky mask should be 274s used, set this parameter to 0. (float; default: 0.05) 274s 274s Calibration frames: ['RAMAN_LINES', 'LSF_PROFILE', 'SKY_MASK'] 274s 274s Raw and product frames: 274s PIXTABLE_OBJECT --> ['RAMAN_IMAGES', 'PIXTABLE_REDUCED'] 274s Author: Ole Streicher 274s 274s 274s Recipe muse_scipost_make_cube: 274s version 2.8.7 274s 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'} 274s Docstring: Make a MUSE cube from a MUSE pixel table. 274s 274s This recipe takes a pixel table and resamples it to either a FITS cube 274s or a Euro3D table and optionally to a stacked spectrum. This is a part 274s of the muse_scipost recipe. 274s 274s Parameters: 274s lambdamin: Cut off the data below this wavelength after loading the 274s pixel table(s). (float; default: 4000.0) 274s lambdamax: Cut off the data above this wavelength after loading the 274s pixel table(s). (float; default: 10000.0) 274s resample: The resampling technique to use for the final output cube. 274s (str; default: 'drizzle') 274s dx: Horizontal step size for resampling (in arcsec or pixel). 274s The following defaults are taken when this value is set to 274s 0.0: 0.2'' for WFM, 0.025'' for NFM, 1.0 if data is in 274s pixel units. (float; default: 0.0) 274s dy: Vertical step size for resampling (in arcsec or pixel). 274s The following defaults are taken when this value is set to 274s 0.0: 0.2'' for WFM, 0.025'' for NFM, 1.0 if data is in 274s pixel units. (float; default: 0.0) 274s dlambda: Wavelength step size (in Angstrom). Natural instrument 274s sampling is used, if this is 0.0 (float; default: 0.0) 274s crtype: Type of statistics used for detection of cosmic rays 274s during final resampling. "iraf" uses the variance 274s information, "mean" uses standard (mean/stdev) statistics, 274s "median" uses median and the median median of the absolute 274s median deviation. (str; default: 'median') 274s crsigma: Sigma rejection factor to use for cosmic ray rejection 274s during final resampling. A zero or negative value switches 274s cosmic ray rejection off. (float; default: 15.0) 274s rc: Critical radius for the "renka" resampling method. (float; 274s default: 1.25) 274s pixfrac: Pixel down-scaling factor for the "drizzle" resampling 274s method. Up to three, comma-separated, floating-point 274s values can be given. If only one value is given, it 274s applies to all dimensions, two values are interpreted as 274s spatial and spectral direction, respectively, while three 274s are taken as horizontal, vertical, and spectral. (str; 274s default: '0.8,0.8') 274s ld: Number of adjacent pixels to take into account during 274s resampling in all three directions (loop distance); this 274s affects all resampling methods except "nearest". (int; 274s default: 1) 274s format: Type of output file format, "Cube" is a standard FITS cube 274s with NAXIS=3 and multiple extensions (for data and 274s variance). The extended "x" formats include the 274s reconstructed image(s) in FITS image extensions within the 274s same file. (str; default: 'Cube') 274s stacked: If true, write an additional output file in form of a 2D 274s stacked image (x direction is pseudo-spatial, y direction 274s is wavelength). (bool; default: False) 274s filter: The filter name(s) to be used for the output field-of-view 274s image. Each name has to correspond to an EXTNAME in an 274s extension of the FILTER_LIST file. If an unsupported 274s filter name is given, creation of the respective image is 274s omitted. If multiple filter names are given, they have to 274s be comma separated. (str; default: 'white') 274s 274s Calibration frames: ['FILTER_LIST', 'OUTPUT_WCS'] 274s 274s Raw and product frames: 274s PIXTABLE_OBJECT --> ['DATACUBE_FINAL', 'IMAGE_FOV', 274s 'OBJECT_RESAMPLED'] 274s Author: Ole Streicher 274s 274s 274s Recipe muse_twilight: 274s version 2.8.7 274s 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} 275s Docstring: Combine several twilight skyflats into one cube, compute correction 275s factors for each IFU, and create a smooth 3D illumination correction. 275s 275s Processing first handles each raw input image separately: it trims the 275s raw data and records the overscan statistics, subtracts the bias 275s (taking account of the overscan, if --overscan is not "none"), 275s converts the images from adu to count, subtracts the dark, divides by 275s the flat-field and combines all the exposures using input parameters. 275s The input calibrations geometry table, trace table, and wavelength 275s calibration table are used to assign 3D coordinates to each CCD-based 275s pixel, thereby creating a pixel table from the master sky-flat. These 275s pixel tables are then cut in wavelength using the --lambdamin and 275s --lambdamax parameters. The integrated flux in each IFU is computed as 275s the sum of the data in the pixel table, and saved in the header, to be 275s used later as estimate for the relative throughput of each IFU. If an 275s ILLUM exposure was given as input, it is then used to correct the 275s relative illumination between all slices of one IFU. For this, the 275s data of each slice within the pixel table of each IFU is multiplied by 275s the normalized median flux of that slice in the ILLUM exposure. The 275s pixel tables of all IFUs are then merged, using the integrated fluxes 275s as inverse scaling factors, and a cube is reconstructed from the 275s merged dataset, using given parameters. A white-light image is created 275s from the cube. This skyflat cube is then saved to disk, with the 275s white-light image as one extension. To construct a smooth 3D 275s illumination correction, the cube is post-processed in the following 275s way: the white-light image is used to create a mask of the illuminated 275s area. From this area, the optional vignetting mask is removed. The 275s smoothing is then computed for each plane of the cube: the illuminated 275s area is smoothed (by a 5x7 median filter), normalized, fit with a 2D 275s polynomial (of given polynomial orders), and normalized again. A 275s smooth white image is then created by collapsing the smooth cube. If a 275s vignetting mask was given or NFM data is processed, an area close to 275s the edge of the MUSE field is used to compute a 2D correction for the 275s vignetted area: the original unsmoothed white-light image is corrected 275s for large scale gradients by dividing it with the smooth white image. 275s The residuals in the edge area (as defined by the input mask or 275s hardcoded for NFM) are then smoothed using input parameters. This 275s smoothed vignetting correction is the multiplied onto each plane of 275s the smooth cube, normalizing each plane again. This twilight cube is 275s then saved to disk. 275s 275s Parameters: 275s overscan: If this is "none", stop when detecting discrepant 275s overscan levels (see ovscsigma), for "offset" it 275s assumes that the mean overscan level represents the 275s real offset in the bias levels of the exposures 275s involved, and adjusts the data accordingly; for 275s "vpoly", a polynomial is fit to the vertical overscan 275s and subtracted from the whole quadrant. (str; default: 275s 'vpoly') 275s ovscreject: This influences how values are rejected when computing 275s overscan statistics. Either no rejection at all 275s ("none"), rejection using the DCR algorithm ("dcr"), 275s or rejection using an iterative constant fit ("fit"). 275s (str; default: 'dcr') 275s ovscsigma: If the deviation of mean overscan levels between a raw 275s input image and the reference image is higher than 275s |ovscsigma x stdev|, stop the processing. If 275s overscan="vpoly", this is used as sigma rejection 275s level for the iterative polynomial fit (the level 275s comparison is then done afterwards with |100 x stdev| 275s to guard against incompatible settings). Has no effect 275s for overscan="offset". (float; default: 30.0) 275s ovscignore: The number of pixels of the overscan adjacent to the 275s data section of the CCD that are ignored when 275s computing statistics or fits. (int; default: 3) 275s combine: Type of combination to use (str; default: 'sigclip') 275s nlow: Number of minimum pixels to reject with minmax (int; 275s default: 1) 275s nhigh: Number of maximum pixels to reject with minmax (int; 275s default: 1) 275s nkeep: Number of pixels to keep with minmax (int; default: 1) 275s lsigma: Low sigma for pixel rejection with sigclip (float; 275s default: 3.0) 275s hsigma: High sigma for pixel rejection with sigclip (float; 275s default: 3.0) 275s scale: Scale the individual images to a common exposure time 275s before combining them. (bool; default: False) 275s resample: The resampling technique to use for the final output 275s cube. (str; default: 'drizzle') 275s crtype: Type of statistics used for detection of cosmic rays 275s during final resampling. "iraf" uses the variance 275s information, "mean" uses standard (mean/stdev) 275s statistics, "median" uses median and the median median 275s of the absolute median deviation. (str; default: 275s 'median') 275s crsigma: Sigma rejection factor to use for cosmic ray rejection 275s during final resampling. A zero or negative value 275s switches cosmic ray rejection off. (float; default: 275s 50.0) 275s lambdamin: Minimum wavelength for twilight reconstruction. 275s (float; default: 5000.0) 275s lambdamax: Maximum wavelength for twilight reconstruction. 275s (float; default: 9000.0) 275s dlambda: Sampling for twilight reconstruction, this should 275s result in planes of equal wavelength coverage. (float; 275s default: 250.0) 275s xorder: Polynomial order to use in x direction to fit the full 275s field of view. (int; default: 2) 275s yorder: Polynomial order to use in y direction to fit the full 275s field of view. (int; default: 2) 275s vignmaskedges: Pixels on edges stronger than this fraction in the 275s normalized image are excluded from the fit to the 275s vignetted area. Set to non-positive number to include 275s them in the fit. This has no effect for NFM skyflats. 275s (float; default: 0.02) 275s vignsmooth: Type of smoothing to use for the vignetted region 275s given by the VIGNETTING_MASK (for WFM, or the internal 275s mask, for NFM); gaussian uses (vignxpar + vignypar)/2 275s as FWHM. (str; default: 'polyfit') 275s vignxpar: Parameter used by the vignetting smoothing: x order 275s for polyfit (default, recommended 4), parameter that 275s influences the FWHM for the gaussian (recommended: 275s 10), or x dimension of median filter (recommended 5). 275s If a negative value is found, the default is taken. 275s (int; default: -1) 275s vignypar: Parameter used by the vignetting smoothing: y order 275s for polyfit (default, recommended 4), parameter that 275s influences the FWHM for the gaussian (recommended: 275s 10), or y dimension of median filter (recommended 5). 275s If a negative value is found, the default is taken. 275s (int; default: -1) 275s vignnfmmask: The height of the vignetted region at the top of the 275s MUSE field in NFM. This is the region modeled 275s separately (the final vignetting model might be 275s smaller). (int; default: 22) 275s 275s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 275s 'BADPIX_TABLE', 'TRACE_TABLE', 'WAVECAL_TABLE', 275s 'GEOMETRY_TABLE', 'VIGNETTING_MASK'] 275s 275s Raw and product frames: 275s SKYFLAT --> ['DATACUBE_SKYFLAT', 'TWILIGHT_CUBE'] 275s ILLUM --> [] 275s Author: Peter Weilbacher 275s 275s 275s Recipe muse_ampl: 275s version 2.8.7 275s 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} 275s Docstring: Determine the instrumental throughput from exposures taken with the 275s pico-amplifier / photo diode readings. 275s 275s This recipe combines several separate amplifier images (flat-fields 275s with special FITS headers containing pico amplifier measurements) into 275s one master image file and computes the instrumental throughput per IFU 275s (and slice). Processing trims the raw data and records the overscan 275s statistics, subtracts the bias (taking account of the overscan, if 275s overscan is not "none"), and optionally, the dark from each raw input 275s image, converts them from adu to count, scales them according to their 275s exposure time, and combines them using input parameters. To compute 275s the throughput the image is converted into a pixel table, the flux is 275s then integrated over the given filter band, and the ratio of the 275s expected flux (FITS header INS.AMPL2.CURR) to measured flux is taken, 275s in the same units. If a geometry table was given as input, the 275s relative area of the IFUs is taken into account when computing the 275s flux per unit area. The resulting ratio is the instrument efficiency 275s (throughput) and saved as QC parameters for the whole input image and 275s per slice in the output pixel table. 275s 275s Parameters: 275s nifu: IFU to handle. If set to 0, all IFUs are processed 275s serially. If set to -1, all IFUs are processed in 275s parallel. (int; default: 0) 275s overscan: If this is "none", stop when detecting discrepant 275s overscan levels (see ovscsigma), for "offset" it assumes 275s that the mean overscan level represents the real offset 275s in the bias levels of the exposures involved, and adjusts 275s the data accordingly; for "vpoly", a polynomial is fit to 275s the vertical overscan and subtracted from the whole 275s quadrant. (str; default: 'vpoly') 275s ovscreject: This influences how values are rejected when computing 275s overscan statistics. Either no rejection at all ("none"), 275s rejection using the DCR algorithm ("dcr"), or rejection 275s using an iterative constant fit ("fit"). (str; default: 275s 'dcr') 275s ovscsigma: If the deviation of mean overscan levels between a raw 275s input image and the reference image is higher than 275s |ovscsigma x stdev|, stop the processing. If 275s overscan="vpoly", this is used as sigma rejection level 275s for the iterative polynomial fit (the level comparison is 275s then done afterwards with |100 x stdev| to guard against 275s incompatible settings). Has no effect for 275s overscan="offset". (float; default: 30.0) 275s ovscignore: The number of pixels of the overscan adjacent to the data 275s section of the CCD that are ignored when computing 275s statistics or fits. (int; default: 3) 275s combine: Type of combination to use (str; default: 'sigclip') 275s nlow: Number of minimum pixels to reject with minmax (int; 275s default: 1) 275s nhigh: Number of maximum pixels to reject with minmax (int; 275s default: 1) 275s nkeep: Number of pixels to keep with minmax (int; default: 1) 275s lsigma: Low sigma for pixel rejection with sigclip (float; 275s default: 3.0) 275s hsigma: High sigma for pixel rejection with sigclip (float; 275s default: 3.0) 275s fbeam: Factor to describe the widening of the beam from the 275s focal plane to photo diode 2. (float; default: 1.1) 275s temp: Lamp temperature [K] used to create the black body 275s function. (float; default: 3200.0) 275s savemaster: Save the processed and combined master image before any 275s concolution is done. (bool; default: False) 275s savetable: Save the table with all the processed pixel values. 275s (bool; default: False) 275s merge: Merge output products from different IFUs into a common 275s file. (bool; default: False) 275s 275s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'BADPIX_TABLE', 275s 'GEOMETRY_TABLE', 'FILTER_LIST', 'TRACE_TABLE', 275s 'WAVECAL_TABLE'] 275s 275s Raw and product frames: 275s AMPL --> ['MASTER_AMPL', 'TABLE_AMPL', 'AMPL_CONVOLVED'] 275s Author: Peter Weilbacher 275s 275s 275s Recipe muse_exp_align: 275s version 2.8.7 275s 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} 275s Docstring: Create a coordinate offset table to be used to align exposures during 275s exposure combination. 275s 275s Compute the coordinate offset for each input field-of-view image with 275s respect to a reference. The created list of coordinate offsets can 275s then be used in muse_exp_combine as the field coordinate offsets to 275s properly align the exposures during their combination. The source 275s positions used to compute the field offsets are obtained by detecting 275s point sources in each of the input images, unless the source detection 275s is overridden and an input source list is available for each input 275s field-of-view image. In this latter case the input source positions 275s are used to calculate the field offsets. 275s 275s Parameters: 275s rsearch: Search radius (in arcsec) for each iteration of 275s the offset computation. (str; default: 275s '30.,4.,2.,0.8') 275s nbins: Number of bins to use for 2D histogram on the 275s first iteration of the offset computation. (int; 275s default: 60) 275s weight: Use weighting. (bool; default: True) 275s fwhm: FWHM in pixels of the convolution filter. (float; 275s default: 5.0) 275s threshold: Initial intensity threshold for detecting point 275s sources. If the value is negative or zero the 275s threshold is taken as sigma above median 275s background MAD. If it is larger than zero the 275s threshold is taken as absolute background level. 275s (float; default: 15.0) 275s bkgignore: Fraction of the image to be ignored. (float; 275s default: 0.05) 275s bkgfraction: Fraction of the image (without the ignored part) 275s to be considered as background. (float; default: 275s 0.1) 275s step: Increment/decrement of the threshold value in 275s subsequent iterations. (float; default: 0.5) 275s iterations: Maximum number of iterations used for detecting 275s sources. (int; default: 100000) 275s srcmin: Minimum number of sources which must be found. 275s (int; default: 5) 275s srcmax: Maximum number of sources which may be found. 275s (int; default: 80) 275s roundmin: Lower limit of the allowed point-source 275s roundness. (float; default: -1.0) 275s roundmax: Upper limit of the allowed point-source 275s roundness. (float; default: 1.0) 275s sharpmin: Lower limit of the allowed point-source 275s sharpness. (float; default: 0.2) 275s sharpmax: Upper limit of the allowed point-source 275s sharpness. (float; default: 1.0) 275s expmap: Enables the creation of a simple exposure map for 275s the combined field- of-view. (bool; default: 275s False) 275s bpixdistance: Minimum allowed distance of a source to the 275s closest bad pixel in pixel. Detected sources 275s which are closer to a bad pixel are not taken 275s into account when computing the field offsets. 275s This option has no effect if the source positions 275s are taken from input catalogs. (float; default: 275s 5.0) 275s override_detection: Overrides the source detection step. If this is 275s enabled and source catalogs are present in the 275s input data set, the source positions used to 275s calculate the field offsets are read from the 275s input catalogs. If no catalogs are available as 275s input data the source positions are detected on 275s the input images. (bool; default: False) 275s 275s Calibration frames: ['SOURCE_LIST'] 275s 275s Raw and product frames: 275s IMAGE_FOV --> ['EXPOSURE_MAP', 'PREVIEW_FOV', 'SOURCE_LIST', 275s 'OFFSET_LIST'] 275s Author: Ralf Palsa 275s 275s 275s Recipe muse_scipost_subtract_sky: 275s version 2.8.7 275s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'orig': '', 'flux_sky': 0.0, 'flux_lamp': 0.0} 275s Docstring: Subtract night sky model. 275s 275s Subtract the sky as defined by the sky lines and continuum from a 275s pixel table. This is a separated task of muse_scipost. 275s 275s Parameters: 275s lambdamin: Cut off the data below this wavelength after loading the 275s pixel table(s). (float; default: 4000.0) 275s lambdamax: Cut off the data above this wavelength after loading the 275s pixel table(s). (float; default: 10000.0) 275s orig: If specified, write an additional column containing the 275s original data to the pixel table. (str; default: '') 275s flux_sky: Reference flat field flux, obtained by sky exposure. This 275s parameter is needed to scale the data of each pixel table 275s if more than one pixel table was used to determine the 275s sky. By default, it is taken from the parameter ESO DRS 275s MUSE FLAT FLUX SKY of the first pixel table. (float; 275s default: 0.0) 275s flux_lamp: Reference flat field flux, obtained by lamp exposure. This 275s parameter is needed to scale the data of each pixel table 275s if more than one pixel table was used to determine the 275s sky. By default, it is taken from the parameter ESO DRS 275s MUSE FLAT FLUX LAMP of the first pixel table. (float; 275s default: 0.0) 275s 275s Calibration frames: ['SKY_LINES', 'SKY_CONTINUUM', 'LSF_PROFILE'] 275s 275s Raw and product frames: 275s PIXTABLE_REDUCED --> ['PIXTABLE_REDUCED'] 275s Author: Ole Streicher 275s 275s 275s Recipe muse_astrometry: 275s version 2.8.7 275s 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'} 275s Docstring: Compute an astrometric solution. 275s 275s Merge pixel tables from all IFUs, apply correction for differential 275s atmospheric refraction (when necessary), optionally apply flux 275s calibration and telluric correction (if the necessary input data was 275s given), and resample the data from all exposures into a datacube. Use 275s the cube to detect objects which are then matched to their reference 275s positions from which a two-dimensional WCS solution is computed. There 275s are two pattern matching algorithm implemented, which can be selected 275s by chosing a positive or zero value of faccuracy. In the first method 275s (with a positive value of faccuracy), start using the search radius, 275s and iteratively decrease it, until no duplicate detections are 275s identified any more. Similarly, iterate the data accuracy (decrease it 275s downwards from the mean positioning error) until matches are found. 275s Remove the remaining unidentified objects. The second method (when 275s faccuracy is set to zero), iterates through all quadruples in both the 275s detected objects and the catalogue, calculates the transformation and 275s checks whether more than 80% of the detections match a catalog entry 275s within the radius. The main output is the ASTROMETRY_WCS file which is 275s a bare FITS header containing the world coordinate solution. The 275s secondary product is DATACUBE_ASTROMETRY, it is not needed for further 275s processing but can be used for verification and debugging. It contains 275s the reconstructed cube and two images created from it in further FITS 275s extensions: a white-light image and the special image created from the 275s central planes of the cube used to detect and centroid the stars (as 275s well as its variance). 275s 275s Parameters: 275s centroid: Centroiding method to use for objects in the field of 275s view. "gaussian" and "moffat" use 2D fits to derive the 275s centroid, "box" is a simple centroid in a square box. 275s (str; default: 'moffat') 275s detsigma: Source detection sigma level to use. If this is negative, 275s values between its absolute and 1.0 are tested with a 275s stepsize of 0.1, to find an optimal solution. (float; 275s default: 1.5) 275s radius: Initial radius in pixels for pattern matching 275s identification in the astrometric field. (float; default: 275s 3.0) 275s faccuracy: Factor of initial accuracy relative to mean positional 275s accuracy of the measured positions to use for pattern 275s matching. If this is set to zero, use the quadruples based 275s method. (float; default: 0.0) 275s niter: Number of iterations of the astrometric fit. (int; 275s default: 2) 275s rejsigma: Rejection sigma level of the astrometric fit. (float; 275s default: 3.0) 275s rotcenter: Center of rotation of the instrument, given as two comma- 275s separated floating point values in pixels. (str; default: 275s '-0.01,-1.20') 275s lambdamin: Cut off the data below this wavelength after loading the 275s pixel table(s). (float; default: 4000.0) 275s lambdamax: Cut off the data above this wavelength after loading the 275s pixel table(s). (float; default: 10000.0) 275s lambdaref: Reference wavelength used for correction of differential 275s atmospheric refraction. The R-band (peak wavelength ~7000 275s Angstrom) that is usually used for guiding, is close to 275s the central wavelength of MUSE, so a value of 7000.0 275s Angstrom should be used if nothing else is known. A value 275s less than zero switches DAR correction off. (float; 275s default: 7000.0) 275s darcheck: Carry out a check of the theoretical DAR correction using 275s source centroiding. If "correct" it will also apply an 275s empirical correction. (str; default: 'none') 275s 275s Calibration frames: ['ASTROMETRY_REFERENCE', 'EXTINCT_TABLE', 275s 'STD_RESPONSE', 'STD_TELLURIC'] 275s 275s Raw and product frames: 275s PIXTABLE_ASTROMETRY --> ['DATACUBE_ASTROMETRY', 'ASTROMETRY_WCS'] 275s Author: Peter Weilbacher 275s 275s 275s Recipe muse_scibasic: 275s version 2.8.7 275s 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} 275s Docstring: Remove the instrumental signature from the data of each CCD and 275s convert them from an image into a pixel table. 275s 275s Processing handles each raw input image separately: it trims the raw 275s data and records the overscan statistics, subtracts the bias (taking 275s account of the overscan, if --overscan is not "none"), optionally 275s detects cosmic rays (note that by default cosmic ray rejection is 275s handled in the post processing recipes while the data is reformatted 275s into a datacube, so that the default setting is cr="none" here), 275s converts the images from adu to count, subtracts the dark, divides by 275s the flat-field, and (optionally) propagates the integrated flux value 275s from the twilight-sky cube. The reduced image is then saved (if 275s --saveimage=true). The input calibrations geometry table, trace table, 275s and wavelength calibration table are used to assign 3D coordinates to 275s each CCD-based pixel, thereby creating a pixel table for each 275s exposure. If --skylines contains one or more wavelengths for (bright 275s and isolated) sky emission lines, these lines are used to correct the 275s wavelength calibration using an offset. The data is then cut to a 275s useful wavelength range (if --crop=true). If an ILLUM exposure was 275s given as input, it is then used to correct the relative illumination 275s between all slices of one IFU. For this, the data of each slice is 275s multiplied by the normalized median flux of that slice in the ILLUM 275s exposure. As last step, the data is divided by the normalized twilight 275s cube (if given), using the 3D coordinate of each pixel in the pixel 275s table to interpolate the twilight correction onto the data. This pre- 275s reduced pixel table for each exposure is then saved to disk. 275s 275s Parameters: 275s nifu: IFU to handle. If set to 0, all IFUs are processed 275s serially. If set to -1, all IFUs are processed in 275s parallel. (int; default: 0) 275s overscan: If this is "none", stop when detecting discrepant 275s overscan levels (see ovscsigma), for "offset" it 275s assumes that the mean overscan level represents the 275s real offset in the bias levels of the exposures 275s involved, and adjusts the data accordingly; for 275s "vpoly", a polynomial is fit to the vertical overscan 275s and subtracted from the whole quadrant. (str; default: 275s 'vpoly') 275s ovscreject: This influences how values are rejected when computing 275s overscan statistics. Either no rejection at all 275s ("none"), rejection using the DCR algorithm ("dcr"), or 275s rejection using an iterative constant fit ("fit"). 275s (str; default: 'dcr') 275s ovscsigma: If the deviation of mean overscan levels between a raw 275s input image and the reference image is higher than 275s |ovscsigma x stdev|, stop the processing. If 275s overscan="vpoly", this is used as sigma rejection level 275s for the iterative polynomial fit (the level comparison 275s is then done afterwards with |100 x stdev| to guard 275s against incompatible settings). Has no effect for 275s overscan="offset". (float; default: 30.0) 275s ovscignore: The number of pixels of the overscan adjacent to the 275s data section of the CCD that are ignored when computing 275s statistics or fits. (int; default: 3) 275s crop: Automatically crop the output pixel tables in 275s wavelength depending on the expected useful wavelength 275s range of the active instrument mode (4750-9350 Angstrom 275s for nominal mode and NFM, 4700-9350 Angstrom for 275s nominal AO mode, and 4600-9350 Angstrom for the 275s extended modes). (bool; default: True) 275s cr: Type of cosmic ray cleaning to use (for quick-look data 275s processing). (str; default: 'none') 275s xbox: Search box size in x. Only used if cr=dcr. (int; 275s default: 15) 275s ybox: Search box size in y. Only used if cr=dcr. (int; 275s default: 40) 275s passes: Maximum number of cleaning passes. Only used if cr=dcr. 275s (int; default: 2) 275s thres: Threshold for detection gap in factors of standard 275s deviation. Only used if cr=dcr. (float; default: 5.8) 275s combine: Type of combination to use. Note that in most cases, 275s science exposures cannot easily be combined on the CCD 275s level, so this should usually be kept as "none"! This 275s does not pay attention about the type of input data, 275s and will combine all raw inputs! (str; default: 'none') 275s nlow: Number of minimum pixels to reject with minmax (int; 275s default: 1) 275s nhigh: Number of maximum pixels to reject with minmax (int; 275s default: 1) 275s nkeep: Number of pixels to keep with minmax (int; default: 1) 275s lsigma: Low sigma for pixel rejection with sigclip (float; 275s default: 3.0) 275s hsigma: High sigma for pixel rejection with sigclip (float; 275s default: 3.0) 275s scale: Scale the individual images to a common exposure time 275s before combining them. (bool; default: True) 275s saveimage: Save the pre-processed CCD-based image of each input 275s exposure before it is transformed into a pixel table. 275s (bool; default: True) 275s skylines: List of wavelengths of sky emission lines (in Angstrom) 275s to use as reference for wavelength offset correction 275s using a Gaussian fit. It can contain multiple 275s (isolated) lines, as comma-separated list, individual 275s shifts are then combined into one weighted average 275s offset. Set to "none" to deactivate. (str; default: 275s '5577.339,6300.304') 275s skyhalfwidth: Half-width of the extraction box (in Angstrom) around 275s each sky emission line. (float; default: 5.0) 275s skybinsize: Size of the bins (in Angstrom per pixel) for the 275s intermediate spectrum to do the Gaussian fit to each 275s sky emission line. (float; default: 0.1) 275s skyreject: Sigma clipping parameters for the intermediate spectrum 275s to do the Gaussian fit to each sky emission line. Up to 275s three comma-separated numbers can be given, which are 275s interpreted as high sigma-clipping limit (float), low 275s limit (float), and number of iterations (integer), 275s respectively. (str; default: '15.,15.,1') 275s resample: Resample the input science data into 2D spectral images 275s using all supplied calibrations for a visual check. 275s Note that the image produced will show small wiggles 275s even when the input calibrations are good and were 275s applied successfully! (bool; default: False) 275s dlambda: Wavelength step (in Angstrom per pixel) to use for 275s resampling. (float; default: 1.25) 275s merge: Merge output products from different IFUs into a common 275s file. (bool; default: False) 275s 275s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 275s 'TRACE_TABLE', 'WAVECAL_TABLE', 'GEOMETRY_TABLE', 275s 'TWILIGHT_CUBE', 'BADPIX_TABLE'] 275s 275s Raw and product frames: 275s OBJECT --> ['OBJECT_RED', 'OBJECT_RESAMPLED', 'PIXTABLE_OBJECT'] 275s STD --> ['STD_RED', 'STD_RESAMPLED', 'PIXTABLE_STD'] 275s SKY --> ['SKY_RED', 'SKY_RESAMPLED', 'PIXTABLE_SKY'] 275s ASTROMETRY --> ['ASTROMETRY_RED', 'ASTROMETRY_RESAMPLED', 275s 'PIXTABLE_ASTROMETRY'] 275s ILLUM --> [] 275s REDUCED --> ['REDUCED_RESAMPLED', 'PIXTABLE_REDUCED'] 275s Author: Peter Weilbacher 275s 275s 275s Recipe muse_scipost_apply_astrometry: 275s version 2.8.7 275s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0} 275s Docstring: Calibrate astrometry for MUSE pixel tables. 275s 275s Apply an astrometric calibration to the pixel table spatial 275s coordinates. This is a task separated from muse_scipost. 275s 275s Parameters: 275s lambdamin: Cut off the data below this wavelength after loading the 275s pixel table(s). (float; default: 4000.0) 275s lambdamax: Cut off the data above this wavelength after loading the 275s pixel table(s). (float; default: 10000.0) 275s 275s Calibration frames: ['ASTROMETRY_WCS'] 275s 275s Raw and product frames: 275s PIXTABLE_OBJECT --> ['PIXTABLE_OBJECT'] 275s Author: Ole Streicher 275s 275s 275s Recipe muse_qi_mask: 275s version 2.8.7 275s Parameters: {'nifu': 0} 275s Docstring: Create image masks for use with the quick image reconstruction. 275s 275s Trace and wavelength calibration tables (24 of them each, one per IFU) 275s are used to build wavelength maps. If the input data is binned, the 275s wavelength maps are binned in the same way (averaging of pixels). The 275s wavelength maps are then thresholded to create masks of the desired 275s wavelength range. Finally, the mask is "untrimmed", i.e. empty regions 275s for the pre- and overscans are added (in a simple way, assuming 275s quadrants of equal size, and padding of 32 pixels on all quadrant 275s edges). Note: this recipe is not part of the main MUSE pipeline but to 275s be used in the integration phase to create image masks until the 275s system is fully qualified. It therefore does only minimal error 275s checking. 275s 275s Parameters: 275s nifu: IFU to handle. If set to 0, all IFUs are processed serially, 275s which is the recommendation for this recipe, since only then 275s all extensions end up in the same output file. (int; default: 275s 0) 275s 275s Calibration frames: ['TRACE_TABLE', 'WAVECAL_TABLE'] 275s 275s Raw and product frames: 275s BIAS --> ['MASK_IMAGE'] 275s Author: Peter Weilbacher 275s 275s 275s Recipe muse_create_sky: 275s version 2.8.7 275s 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} 275s Docstring: Create night sky model from selected pixels of an exposure of empty 275s sky. 275s 275s This recipe creates the continuum and the atmospheric transition line 275s spectra of the night sky from the data in a pixel table(s) belonging 275s to one exposure of (mostly) empty sky. 275s 275s Parameters: 275s fraction: Fraction of the image (without the ignored part) to be 275s considered as sky. If an input sky mask is provided, the 275s fraction is applied to the regions within the mask. If the 275s whole sky mask should be used, set this parameter to 1. 275s (float; default: 0.75) 275s ignore: Fraction of the image to be ignored. If an input sky mask 275s is provided, the fraction is applied to the regions within 275s the mask. If the whole sky mask should be used, set this 275s parameter to 0. (float; default: 0.05) 275s sampling: Spectral sampling of the sky spectrum [Angstrom]. (float; 275s default: 0.3125) 275s csampling: Spectral sampling of the continuum spectrum [Angstrom]. 275s (float; default: 0.3125) 275s crsigma: Sigma level clipping for cube-based and spectrum-based CR 275s rejection. This has to be a string of two comma-separated 275s floating-point numbers. The first value gives the sigma- 275s level rejection for cube-based CR rejection (using 275s "median", see muse_scipost), the second value the sigma- 275s level for spectrum-based CR cleaning. Both can be switched 275s off, by passing zero or a negative value. (str; default: 275s '15.,15.') 275s lambdamin: Cut off the data below this wavelength after loading the 275s pixel table(s). (float; default: 4000.0) 275s lambdamax: Cut off the data above this wavelength after loading the 275s pixel table(s). (float; default: 10000.0) 275s lambdaref: Reference wavelength used for correction of differential 275s atmospheric refraction. The R-band (peak wavelength ~7000 275s Angstrom) that is usually used for guiding, is close to 275s the central wavelength of MUSE, so a value of 7000.0 275s Angstrom should be used if nothing else is known. A value 275s less than zero switches DAR correction off. (float; 275s default: 7000.0) 275s 275s Calibration frames: ['EXTINCT_TABLE', 'STD_RESPONSE', 'STD_TELLURIC', 275s 'SKY_LINES', 'SKY_CONTINUUM', 'LSF_PROFILE', 275s 'SKY_MASK'] 275s 275s Raw and product frames: 275s PIXTABLE_SKY --> ['SKY_MASK', 'SKY_IMAGE', 'SKY_SPECTRUM', 275s 'SKY_LINES', 'SKY_CONTINUUM'] 275s Author: Ole Streicher 275s 275s 275s Recipe muse_scipost_correct_rv: 275s version 2.8.7 275s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'rvcorr': 'bary'} 275s Docstring: Apply RV correction for MUSE pixel tables. 275s 275s Correct the wavelengths in the pixel table by given radial-velocity 275s correction. This is a task separated from muse_scipost. 275s 275s Parameters: 275s lambdamin: Cut off the data below this wavelength after loading the 275s pixel table(s). (float; default: 4000.0) 275s lambdamax: Cut off the data above this wavelength after loading the 275s pixel table(s). (float; default: 10000.0) 275s rvcorr: Correct the radial velocity of the telescope with 275s reference to either the barycenter of the Solar System 275s (bary), the center of the Sun (helio), or to the center of 275s the Earth (geo). (str; default: 'bary') 275s 275s Calibration frames: [] 275s 275s Raw and product frames: 275s PIXTABLE_OBJECT --> ['PIXTABLE_REDUCED'] 275s Author: Peter Weilbacher 275s 275s 275s Recipe muse_scipost: 275s version 2.8.7 275s 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} 275s Docstring: Prepare reduced and combined science products. 275s 275s Sort input pixel tables into lists of files per exposure, merge pixel 275s tables from all IFUs of each exposure. Correct each exposure for 275s differential atmospheric refraction (unless --lambdaref is far outside 275s the MUSE wavelength range, or NFM is used which has a built-in 275s corrector). Then the flux calibration is carried out, if a response 275s curve was given in the input; it includes a correction of telluric 275s absorption, if a telluric absorption correction file was given. If 275s observations were done with AO and a RAMAN_LINES file was given, a 275s procedure is run to clean the Raman scattering emission lines from the 275s data. Next, the slice autocalibration is computed and the flux 275s correction factors are applied to the pixel table (if 275s --autocalib="deepfield"). If user-provided autocalibration is 275s requested (--autocalib="user"), then the autocalibration is not 275s computed on the input exposure but the autocalibration factors are 275s read from the AUTOCAL_FACTORS table and applied directly to the data. 275s Then the sky subtraction is carried out (unless --skymethod="none"), 275s either directly subtracting an input sky continuum and an input sky 275s emission lines (for --skymethod="subtract-model"), or 275s (--skymethod="model") create a sky spectrum from the darkest fraction 275s (--skymodel_fraction, after ignoring the lowest --skymodel_ignore as 275s artifacts) of the field of view, then fitting and subtracting sky 275s emission lines using an initial estimate of the input sky lines; then 275s the continuum (residuals after subtracting the sky lines from the sky 275s spectrum) is subtracted as well. If --save contains "skymodel", all 275s sky-related products are saved for each exposure. Afterwards the data 275s is corrected for the radial velocity of the observer (--rvcorr), 275s before the input (or a default) astrometric solution is applied. Now 275s each individual exposure is fully reduced; the pixel tables at this 275s stage can be saved by setting "individual" in --save. If multiple 275s exposures were given, they are then combined. If --save contains 275s "combined", this final merged pixel table is saved. Finally (if --save 275s contains "cube"), the data is resampled into a datacube, using all 275s parameters given to the recipe. The extent and orientation of the cube 275s is normally computed from the data itself, but this can be overridden 275s by passing a file with the output world coordinate system 275s (OUTPUT_WCS), for example a MUSE cube. This can also be used to sample 275s the wavelength axis logarithmically (in that file set "CTYPE3='AWAV- 275s LOG'"). As a last step, the computed cube is integrated over all 275s filter functions given (--filter) that are also present in the input 275s filter list table. 275s 275s Parameters: 275s save: Select output product(s) to save. Can contain one 275s or more of "cube", "autocal", "skymodel", 275s "individual", "positioned", "combined", and 275s "stacked". If several options are given, they 275s have to be comma- separated. ("cube": output cube 275s and associated images, if this is not given, no 275s final resampling is done at all -- "autocal": up 275s to two additional output products related to the 275s slice autocalibration -- "raman": up to four 275s additional output products about the Raman light 275s distribution for AO observations -- "skymodel": 275s up to four additional output products about the 275s effectively used sky that was subtracted with the 275s "model" method -- "individual": fully reduced 275s pixel table for each individual exposure -- 275s "positioned": fully reduced and positioned pixel 275s table for each individual exposure, the 275s difference to "individual" is that here, the 275s output pixel tables have coordinates in RA and 275s DEC, and the optional offsets were applied; this 275s is only useful, if both the relative exposure 275s weighting and the final resampling are to be done 275s externally -- "combined": fully reduced and 275s combined pixel table for the full set of 275s exposures, the difference to "positioned" is that 275s all pixel tables are combined into one, with an 275s added weight column; this is useful, if only the 275s final resampling step is to be done separately -- 275s "stacked": an additional output file in form of a 275s 2D column-stacked image, i.e. x direction is 275s pseudo-spatial, y direction is wavelength.) (str; 275s default: 'cube,skymodel') 275s resample: The resampling technique to use for the final 275s output cube. (str; default: 'drizzle') 275s dx: Horizontal step size for resampling (in arcsec or 275s pixel). The following defaults are taken when 275s this value is set to 0.0: 0.2'' for WFM, 0.025'' 275s for NFM, 1.0 if data is in pixel units. (float; 275s default: 0.0) 275s dy: Vertical step size for resampling (in arcsec or 275s pixel). The following defaults are taken when 275s this value is set to 0.0: 0.2'' for WFM, 0.025'' 275s for NFM, 1.0 if data is in pixel units. (float; 275s default: 0.0) 275s dlambda: Wavelength step size (in Angstrom). Natural 275s instrument sampling is used, if this is 0.0 275s (float; default: 0.0) 275s crtype: Type of statistics used for detection of cosmic 275s rays during final resampling. "iraf" uses the 275s variance information, "mean" uses standard 275s (mean/stdev) statistics, "median" uses median and 275s the median median of the absolute median 275s deviation. (str; default: 'median') 275s crsigma: Sigma rejection factor to use for cosmic ray 275s rejection during final resampling. A zero or 275s negative value switches cosmic ray rejection off. 275s (float; default: 15.0) 275s rc: Critical radius for the "renka" resampling 275s method. (float; default: 1.25) 275s pixfrac: Pixel down-scaling factor for the "drizzle" 275s resampling method. Up to three, comma-separated, 275s floating-point values can be given. If only one 275s value is given, it applies to all dimensions, two 275s values are interpreted as spatial and spectral 275s direction, respectively, while three are taken as 275s horizontal, vertical, and spectral. (str; 275s default: '0.8,0.8') 275s ld: Number of adjacent pixels to take into account 275s during resampling in all three directions (loop 275s distance); this affects all resampling methods 275s except "nearest". (int; default: 1) 275s format: Type of output file format, "Cube" is a standard 275s FITS cube with NAXIS=3 and multiple extensions 275s (for data and variance). The extended "x" formats 275s include the reconstructed image(s) in FITS image 275s extensions within the same file. "sdpCube" does 275s some extra calculations to create FITS keywords 275s for the ESO Science Data Products. (str; default: 275s 'Cube') 275s weight: Type of weighting scheme to use when combining 275s multiple exposures. "exptime" just uses the 275s exposure time to weight the exposures, "fwhm" 275s uses the best available seeing information from 275s the headers as well, "none" preserves an existing 275s weight column in the input pixel tables without 275s changes. (str; default: 'exptime') 275s filter: The filter name(s) to be used for the output 275s field-of-view image. Each name has to correspond 275s to an EXTNAME in an extension of the FILTER_LIST 275s file. If an unsupported filter name is given, 275s creation of the respective image is omitted. If 275s multiple filter names are given, they have to be 275s comma separated. (str; default: 'white') 275s autocalib: The type of autocalibration to use. "none" 275s switches it off, "deepfield" uses the revised 275s MPDAF method that can be used for the reduction 275s of mostly empty "Deep Fields", "user" searches 275s for a user- provided table with autocalibration 275s factors. (str; default: 'none') 275s raman_width: Wavelength range around Raman lines [Angstrom]. 275s (float; default: 20.0) 275s skymethod: The method used to subtract the sky background 275s (spectrum). Option "model" should work in all 275s kinds of science fields: it uses a global sky 275s spectrum model with a local LSF. "model" uses 275s fluxes indicated in the SKY_LINES file as 275s starting estimates, but re-fits them on the 275s global sky spectrum created from the science 275s exposure. If SKY_CONTINUUM is given, it is 275s directly subtracted, otherwise it is created from 275s the sky region of the science exposure. Option 275s "subtract- model" uses the input SKY_LINES and 275s SKY_CONTINUUM, subtracting them directly without 275s re-fitting the fluxes, but still makes use of the 275s local LSF, hence LSF_PROFILE is required. The 275s inputs LSF_PROFILE and SKY_LINES are necessary 275s for these two model-based methods; SKY_CONTINUUM 275s is required for "subtract-model" and optional for 275s "model"; SKY_MASK is optional for "model". 275s Finally, option "simple" creates a sky spectrum 275s from the science data, and directly subtracts it, 275s without taking the LSF into account (LSF_PROFILE 275s and input SKY files are ignored). It works on 275s data that was not flux calibrated. (str; default: 275s 'model') 275s lambdamin: Cut off the data below this wavelength after 275s loading the pixel table(s). (float; default: 275s 4000.0) 275s lambdamax: Cut off the data above this wavelength after 275s loading the pixel table(s). (float; default: 275s 10000.0) 275s lambdaref: Reference wavelength used for correction of 275s differential atmospheric refraction. The R-band 275s (peak wavelength ~7000 Angstrom) that is usually 275s used for guiding, is close to the central 275s wavelength of MUSE, so a value of 7000.0 Angstrom 275s should be used if nothing else is known. A value 275s less than zero switches DAR correction off. 275s (float; default: 7000.0) 275s darcheck: Carry out a check of the theoretical DAR 275s correction using source centroiding. If "correct" 275s it will also apply an empirical correction. (str; 275s default: 'none') 275s skymodel_fraction: Fraction of the image (without the ignored part) 275s to be considered as sky. If an input sky mask is 275s provided, the fraction is applied to the regions 275s within the mask. If the whole sky mask should be 275s used, set this parameter to 1. (float; default: 275s 0.1) 275s skymodel_ignore: Fraction of the image to be ignored. If an input 275s sky mask is provided, the fraction is applied to 275s the regions within the mask. If the whole sky 275s mask should be used, set this parameter to 0. 275s (float; default: 0.05) 275s skymodel_sampling: Spectral sampling of the sky spectrum [Angstrom]. 275s (float; default: 0.3125) 275s skymodel_csampling: Spectral sampling of the continuum spectrum 275s [Angstrom]. (float; default: 0.3125) 275s sky_crsigma: Sigma level clipping for cube-based and spectrum- 275s based CR rejection when creating the sky 275s spectrum. This has to be a string of two comma- 275s separated floating-point numbers. The first value 275s gives the sigma- level rejection for cube-based 275s CR rejection (using "median"), the second value 275s the sigma-level for spectrum-based CR cleaning. 275s Both can be switched off, by passing zero or a 275s negative value. (str; default: '15.,15.') 275s rvcorr: Correct the radial velocity of the telescope with 275s reference to either the barycenter of the Solar 275s System (bary), the center of the Sun (helio), or 275s to the center of the Earth (geo). (str; default: 275s 'bary') 275s astrometry: If false, skip any astrometric calibration, even 275s if one was passed in the input set of files. This 275s causes creation of an output cube with a linear 275s WCS and may result in errors. If you want to use 275s a sensible default, leave this true but do not 275s pass an ASTROMETRY_WCS. (bool; default: True) 275s 275s Calibration frames: ['EXTINCT_TABLE', 'STD_RESPONSE', 'STD_TELLURIC', 275s 'ASTROMETRY_WCS', 'OFFSET_LIST', 'FILTER_LIST', 275s 'OUTPUT_WCS', 'AUTOCAL_FACTORS', 'RAMAN_LINES', 275s 'SKY_LINES', 'SKY_CONTINUUM', 'LSF_PROFILE', 275s 'SKY_MASK'] 275s 275s Raw and product frames: 275s PIXTABLE_OBJECT --> ['DATACUBE_FINAL', 'IMAGE_FOV', 275s 'OBJECT_RESAMPLED', 'PIXTABLE_REDUCED', 275s 'PIXTABLE_POSITIONED', 'PIXTABLE_COMBINED', 275s 'AUTOCAL_MASK', 'AUTOCAL_FACTORS', 275s 'RAMAN_IMAGES', 'SKY_IMAGE', 'SKY_MASK', 275s 'SKY_SPECTRUM', 'SKY_LINES', 'SKY_CONTINUUM'] 275s Author: Peter Weilbacher 275s 275s 275s Recipe muse_exp_combine: 275s version 2.8.7 275s 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} 275s Docstring: Combine several exposures into one datacube. 275s 275s Sort reduced pixel tables, one per exposure, by exposure and combine 275s them with applied weights into one final datacube. 275s 275s Parameters: 275s save: Select output product(s) to save. Can contain one or more 275s of "cube" (output cube and associated images; if this is 275s not given, no resampling is done at all) or "combined" 275s (fully reduced and combined pixel table for the full set 275s of exposures; this is useful, if the final resampling step 275s is to be done again separately). If several options are 275s given, they have to be comma-separated. (str; default: 275s 'cube') 275s resample: The resampling technique to use for the final output cube. 275s (str; default: 'drizzle') 275s dx: Horizontal step size for resampling (in arcsec or pixel). 275s The following defaults are taken when this value is set to 275s 0.0: 0.2'' for WFM, 0.025'' for NFM, 1.0 if data is in 275s pixel units. (float; default: 0.0) 275s dy: Vertical step size for resampling (in arcsec or pixel). 275s The following defaults are taken when this value is set to 275s 0.0: 0.2'' for WFM, 0.025'' for NFM, 1.0 if data is in 275s pixel units. (float; default: 0.0) 275s dlambda: Wavelength step size (in Angstrom). Natural instrument 275s sampling is used, if this is 0.0 (float; default: 0.0) 275s crtype: Type of statistics used for detection of cosmic rays 275s during final resampling. "iraf" uses the variance 275s information, "mean" uses standard (mean/stdev) statistics, 275s "median" uses median and the median median of the absolute 275s median deviation. (str; default: 'median') 275s crsigma: Sigma rejection factor to use for cosmic ray rejection 275s during final resampling. A zero or negative value switches 275s cosmic ray rejection off. (float; default: 10.0) 275s rc: Critical radius for the "renka" resampling method. (float; 275s default: 1.25) 275s pixfrac: Pixel down-scaling factor for the "drizzle" resampling 275s method. Up to three, comma-separated, floating-point 275s values can be given. If only one value is given, it 275s applies to all dimensions, two values are interpreted as 275s spatial and spectral direction, respectively, while three 275s are taken as horizontal, vertical, and spectral. (str; 275s default: '0.6,0.6') 275s ld: Number of adjacent pixels to take into account during 275s resampling in all three directions (loop distance); this 275s affects all resampling methods except "nearest". (int; 275s default: 1) 275s format: Type of output file format, "Cube" is a standard FITS cube 275s with NAXIS=3 and multiple extensions (for data and 275s variance). The extended "x" formats include the 275s reconstructed image(s) in FITS image extensions within the 275s same file. "sdpCube" does some extra calculations to 275s create FITS keywords for the ESO Science Data Products. 275s (str; default: 'Cube') 275s weight: Type of weighting scheme to use when combining multiple 275s exposures. "exptime" just uses the exposure time to weight 275s the exposures, "fwhm" uses the best available seeing 275s information from the headers as well, "header" queries 275s ESO.DRS.MUSE.WEIGHT of each input file instead of the 275s FWHM, and "none" preserves an existing weight column in 275s the input pixel tables without changes. (str; default: 275s 'exptime') 275s filter: The filter name(s) to be used for the output field-of-view 275s image. Each name has to correspond to an EXTNAME in an 275s extension of the FILTER_LIST file. If an unsupported 275s filter name is given, creation of the respective image is 275s omitted. If multiple filter names are given, they have to 275s be comma separated. (str; default: 'white') 275s lambdamin: Cut off the data below this wavelength after loading the 275s pixel table(s). (float; default: 4000.0) 275s lambdamax: Cut off the data above this wavelength after loading the 275s pixel table(s). (float; default: 10000.0) 275s 275s Calibration frames: ['OFFSET_LIST', 'FILTER_LIST', 'OUTPUT_WCS'] 275s 275s Raw and product frames: 275s PIXTABLE_REDUCED --> ['DATACUBE_FINAL', 'IMAGE_FOV', 275s 'PIXTABLE_COMBINED'] 275s Author: Peter Weilbacher 275s 275s 275s Recipe muse_scipost_subtract_sky_simple: 275s version 2.8.7 275s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0} 275s Docstring: Subtract night sky spectrum. 275s 275s Subtract the sky in a simple way, just using a sky spectrum created by 275s muse_create_sky. This is a separated task of muse_scipost. 275s 275s Parameters: 275s lambdamin: Cut off the data below this wavelength after loading the 275s pixel table(s). (float; default: 4000.0) 275s lambdamax: Cut off the data above this wavelength after loading the 275s pixel table(s). (float; default: 10000.0) 275s 275s Calibration frames: ['SKY_SPECTRUM'] 275s 275s Raw and product frames: 275s PIXTABLE_REDUCED --> ['PIXTABLE_REDUCED'] 275s Author: Peter Weilbacher 275s 275s 275s Recipe muse_lingain: 275s version 2.8.7 275s 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} 275s Docstring: Compute the gain and a model of the residual non-linearity for each 275s detector quadrant 275s 275s The recipe uses the bias and flat field images of a detector 275s monitoring exposure sequence to determine the detector gain in 275s counts/ADU and to model the residual non-linearity for each of the 275s four detector quadrants of all IFUs. All measurements done by the 275s recipe are done on the illuminated parts of the detector, i.e. on the 275s slices. The location of the slices is taken from the given trace 275s table, which is a mandatory input. Using the traces of the slices on 275s the detector a set of measurement windows is placed along these 275s traces. The data used for the determination of the gain and the 275s residual non-linearity is the taken from these windows. Bad pixels 275s indicated by an, optionally, provided bad pixel table, or flagged 275s during the preprocessing (bias subtraction) of the input data are 275s excluded from the measurements. Local measurements of the read-out- 275s noise, the signal and the gain are calculated for each of the 275s measurement windows. Using these measurements the gain for each 275s detector quadrant is computed as the zero-order coefficient of a 1st 275s order polynomial fitted to the binned gain measurements as a function 275s of the signal level. The residual non-linearity is modelled by a 275s (high) order polynomial which is fitted to the fractional percentage 275s deviation of the count rate from an expected constant count rate (the 275s linear case) as function of the signal level. (Not yet implemented!) 275s 275s Parameters: 275s nifu: IFU to handle. If set to 0, all IFUs are processed 275s serially. If set to -1, all IFUs are processed in 275s parallel. (int; default: 0) 275s ybox: Size of windows along the traces of the slices. (int; 275s default: 50) 275s xgap: Extra offset from tracing edge. (int; default: 3) 275s xborder: Extra offset from the detector edge used for the selection 275s of slices. (int; default: 10) 275s order: Order of the polynomial used to fit the non-linearity 275s residuals. (int; default: 12) 275s toffset: Exposure time offset in seconds to apply to linearity flat 275s fields. (float; default: 0.018) 275s fluxtol: Tolerance value for the overall flux consistency check of 275s a pair of flat fields. The value is the maximum relative 275s offset. (float; default: 0.01) 275s sigma: Sigma value used for signal value clipping. (float; 275s default: 3.0) 275s signalmin: Minimum signal value in log(ADU) used for the gain 275s analysis and the non-linearity polynomial model. (float; 275s default: 0.0) 275s signalmax: Maximum signal value in log(ADU) used for the gain 275s analysis and the non-linearity polynomial model. (float; 275s default: 4.9) 275s signalbin: Size of a signal bin in log10(ADU) used for the gain 275s analysis and the non-linearity polynomial model. (float; 275s default: 0.1) 275s gainlimit: Minimum signal value [ADU] used for fitting the gain 275s relation. (float; default: 100.0) 275s gainsigma: Sigma value for gain value clipping. (float; default: 3.0) 275s ctsmin: Minimum signal value in log(counts) to consider for the 275s non-linearity analysis. (float; default: 3.0) 275s ctsmax: Maximum signal value in log(counts) to consider for the 275s non-linearity analysis. (float; default: 4.9) 275s ctsbin: Size of a signal bin in log10(counts) used for the non- 275s linearity analysis. (float; default: 0.1) 275s linearmin: Lower limit of desired linear range in log10(counts). 275s (float; default: 2.5) 275s linearmax: Upper limit of desired linear range in log10(counts). 275s (float; default: 3.0) 275s merge: Merge output products from different IFUs into a common 275s file. (bool; default: False) 275s 275s Calibration frames: ['MASTER_BIAS', 'TRACE_TABLE', 'BADPIX_TABLE'] 275s 275s Raw and product frames: 275s LINGAIN_LAMP_OFF --> ['NONLINEARITY_GAIN'] 275s LINGAIN_LAMP_ON --> ['NONLINEARITY_GAIN'] 275s Author: Ralf Palsa 275s 275s 275s Recipe muse_scipost_combine_pixtables: 275s version 2.8.7 275s Parameters: {'lambdamin': 4000.0, 'lambdamax': 10000.0, 'weight': 'exptime'} 275s Docstring: Combine MUSE pixel tables, either from different IFUs, or from 275s different exposures, or both. 275s 275s Sort pixel tables by exposure and combine them with applied weights 275s into one big pixel table. This is a task separated from muse_scipost. 275s 275s Parameters: 275s lambdamin: Cut off the data below this wavelength after loading the 275s pixel table(s). (float; default: 4000.0) 275s lambdamax: Cut off the data above this wavelength after loading the 275s pixel table(s). (float; default: 10000.0) 275s weight: Type of weighting scheme to use when combining multiple 275s exposures. "exptime" just uses the exposure time to weight 275s the exposures, "fwhm" uses the DIMM information in the 275s header as well, "none" preserves an existing weight column 275s in the input pixel tables without changes. (str; default: 275s 'exptime') 275s 275s Calibration frames: ['OFFSET_LIST'] 275s 275s Raw and product frames: 275s PIXTABLE_OBJECT --> ['PIXTABLE_COMBINED'] 275s Author: Ole Streicher 275s 275s 275s Recipe muse_wavecal: 275s version 2.8.7 275s 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} 275s Docstring: Detect arc emission lines and determine the wavelength solution for 275s each slice. 275s 275s This recipe detects arc emission lines and fits a wavelength solution 275s to each slice of the instrument. The wavelength calibration table 275s contains polynomials defining the wavelength solution of the slices on 275s the CCD. Processing trims the raw data and records the overscan 275s statistics, subtracts the bias (taking account of the overscan, if 275s --overscan is not "none") and converts them from adu to count. 275s Optionally, the dark can be subtracted and the data can be divided by 275s the flat-field, but this is not recommended. The data is then combined 275s using input parameters, into separate images for each lamp. To compute 275s the wavelength solution, arc lines are detected at the center of each 275s slice (using threshold detection on a S/N image) and subsequently 275s assigned wavelengths, using pattern matching to identify lines from 275s the input line catalog. Each line is then traced to the edges of the 275s slice, using Gaussian centering in each CCD column. The Gaussians not 275s only yield center, but also centering error, and line properties (e.g. 275s FWHM). Deviant fits are detected using polynomial fits to each arc 275s line (using the xorder parameter) and rejected. These analysis and 275s measuring steps are carried out separately on images exposed by the 275s different arc lamps, reducing the amount of blending, that can 275s otherwise influence line identification and Gaussian centering. The 275s final two-dimensional fit uses all positions (of all lamps), their 275s wavelengths, and the given polynomial orders to compute the final 275s wavelength solution for each slice, iteratively rejecting outliers. 275s This final fit can be either unweighted (fitweighting="uniform", for 275s fastest processing) or weighted (other values of fitweighting, for 275s higher accuracy). 275s 275s Parameters: 275s nifu: IFU to handle. If set to 0, all IFUs are processed 275s serially. If set to -1, all IFUs are processed in 275s parallel. (int; default: 0) 275s overscan: If this is "none", stop when detecting discrepant 275s overscan levels (see ovscsigma), for "offset" it 275s assumes that the mean overscan level represents the 275s real offset in the bias levels of the exposures 275s involved, and adjusts the data accordingly; for 275s "vpoly", a polynomial is fit to the vertical overscan 275s and subtracted from the whole quadrant. (str; default: 275s 'vpoly') 275s ovscreject: This influences how values are rejected when computing 275s overscan statistics. Either no rejection at all 275s ("none"), rejection using the DCR algorithm ("dcr"), or 275s rejection using an iterative constant fit ("fit"). 275s (str; default: 'dcr') 275s ovscsigma: If the deviation of mean overscan levels between a raw 275s input image and the reference image is higher than 275s |ovscsigma x stdev|, stop the processing. If 275s overscan="vpoly", this is used as sigma rejection level 275s for the iterative polynomial fit (the level comparison 275s is then done afterwards with |100 x stdev| to guard 275s against incompatible settings). Has no effect for 275s overscan="offset". (float; default: 30.0) 275s ovscignore: The number of pixels of the overscan adjacent to the 275s data section of the CCD that are ignored when computing 275s statistics or fits. (int; default: 3) 275s combine: Type of lampwise image combination to use. (str; 275s default: 'sigclip') 275s lampwise: Identify and measure the arc emission lines on images 275s separately for each lamp setup. (bool; default: True) 275s sigma: Sigma level used to detect arc emission lines above the 275s median background level in the S/N image of the central 275s column of each slice (float; default: 1.0) 275s dres: The allowed range of resolutions for pattern matching 275s (of detected arc lines to line list) in fractions 275s relative to the expected value (float; default: 0.05) 275s tolerance: Tolerance for pattern matching (of detected arc lines 275s to line list) (float; default: 0.1) 275s xorder: Order of the polynomial for the horizontal curvature 275s within each slice (int; default: 2) 275s yorder: Order of the polynomial used to fit the dispersion 275s relation (int; default: 6) 275s linesigma: Sigma level for iterative rejection of deviant fits for 275s each arc line within each slice, a negative value means 275s to use the default (2.5). (float; default: -1.0) 275s residuals: Create a table containing residuals of the fits to the 275s data of all arc lines. This is useful to assess the 275s quality of the wavelength solution in detail. (bool; 275s default: False) 275s fitsigma: Sigma level for iterative rejection of deviant 275s datapoints during the final polynomial wavelength 275s solution within each slice, a negative value means to 275s use the default (3.0). (float; default: -1.0) 275s fitweighting: Type of weighting to use in the final polynomial 275s wavelength solution fit, using centroiding error 275s estimate and/or scatter of each single line as 275s estimates of its accuracy. (str; default: 275s 'cerrscatter') 275s saveimages: Save (bool; default: False) 275s resample: Resample the input arc images onto 2D images for a 275s visual check using tracing and wavelength calibration 275s solutions. Note that the image produced will show small 275s wiggles even when the calibration was successful! 275s (bool; default: False) 275s wavemap: Create a wavelength map of the input images (bool; 275s default: False) 275s merge: Merge output products from different IFUs into a common 275s file. (bool; default: False) 275s 275s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'MASTER_FLAT', 275s 'TRACE_TABLE', 'LINE_CATALOG', 'BADPIX_TABLE'] 275s 275s Raw and product frames: 275s ARC --> ['WAVECAL_TABLE', 'WAVECAL_RESIDUALS', 'ARC_RED_LAMP'] 275s Author: Peter Weilbacher 275s 275s 275s Recipe muse_flat: 275s version 2.8.7 275s 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} 275s Docstring: Combine several separate flat images into one master flat file, trace 275s slice locations, and locate dark pixels. 275s 275s This recipe combines several separate flat-field images into one 275s master flat-field file and traces the location of the slices on the 275s CCD. The master flat contains the combined pixel values of the raw 275s flat exposures, with respect to the image combination method used, 275s normalized to the mean flux. The trace table contains polynomials 275s defining the location of the slices on the CCD. Processing trims the 275s raw data and records the overscan statistics, subtracts the bias 275s (taking account of the overscan, if --overscan is not "none"), and 275s optionally, the dark from each raw input image, converts them from adu 275s to count, scales them according to their exposure time, and combines 275s the exposures using input parameters. To trace the position of the 275s slices on the CCD, their edges are located using a threshold method. 275s The edge detection is repeated at given intervals thereby tracing the 275s central position (the mean of both edges) and width of each slit 275s vertically across the CCD. Deviant positions of detections on CCD rows 275s can be detected and excluded before fitting a polynomial to all 275s positions measured for one slice. The polynomial parameters for each 275s slice are saved in the output trace table. Finally, the area between 275s the now known slice edges is searched for dark (and bright) pixels, 275s using statistics in each row of the master flat. 275s 275s Parameters: 275s nifu: IFU to handle. If set to 0, all IFUs are processed 275s serially. If set to -1, all IFUs are processed in 275s parallel. (int; default: 0) 275s overscan: If this is "none", stop when detecting discrepant 275s overscan levels (see ovscsigma), for "offset" it 275s assumes that the mean overscan level represents the 275s real offset in the bias levels of the exposures 275s involved, and adjusts the data accordingly; for 275s "vpoly", a polynomial is fit to the vertical overscan 275s and subtracted from the whole quadrant. (str; default: 275s 'vpoly') 275s ovscreject: This influences how values are rejected when computing 275s overscan statistics. Either no rejection at all 275s ("none"), rejection using the DCR algorithm ("dcr"), 275s or rejection using an iterative constant fit ("fit"). 275s (str; default: 'dcr') 275s ovscsigma: If the deviation of mean overscan levels between a raw 275s input image and the reference image is higher than 275s |ovscsigma x stdev|, stop the processing. If 275s overscan="vpoly", this is used as sigma rejection 275s level for the iterative polynomial fit (the level 275s comparison is then done afterwards with |100 x stdev| 275s to guard against incompatible settings). Has no effect 275s for overscan="offset". (float; default: 30.0) 275s ovscignore: The number of pixels of the overscan adjacent to the 275s data section of the CCD that are ignored when 275s computing statistics or fits. (int; default: 3) 275s combine: Type of combination to use (str; default: 'sigclip') 275s nlow: Number of minimum pixels to reject with minmax (int; 275s default: 1) 275s nhigh: Number of maximum pixels to reject with minmax (int; 275s default: 1) 275s nkeep: Number of pixels to keep with minmax (int; default: 1) 275s lsigma: Low sigma for pixel rejection with sigclip (float; 275s default: 3.0) 275s hsigma: High sigma for pixel rejection with sigclip (float; 275s default: 3.0) 275s scale: Scale the individual images to a common exposure time 275s before combining them. (bool; default: True) 275s normalize: Normalize the master flat to the average flux (bool; 275s default: True) 275s trace: Trace the position of the slices on the master flat 275s (bool; default: True) 275s nsum: Number of lines over which to average when tracing 275s (int; default: 32) 275s order: Order of polynomial fit to the trace (int; default: 5) 275s edgefrac: Fractional change required to identify edge when 275s tracing (float; default: 0.5) 275s losigmabadpix: Low sigma to find dark pixels in the master flat 275s (float; default: 5.0) 275s hisigmabadpix: High sigma to find bright pixels in the master flat 275s (float; default: 5.0) 275s samples: Create a table containing all tracing sample points. 275s (bool; default: False) 275s merge: Merge output products from different IFUs into a 275s common file. (bool; default: False) 275s 275s Calibration frames: ['MASTER_BIAS', 'MASTER_DARK', 'BADPIX_TABLE'] 275s 275s Raw and product frames: 275s FLAT --> ['MASTER_FLAT', 'TRACE_TABLE', 'TRACE_SAMPLES'] 275s Author: Peter Weilbacher (based on Joris Gerssen's draft) 275s 275s 275s autopkgtest [00:39:20]: test test-recipe.py: -----------------------] 275s autopkgtest [00:39:20]: test test-recipe.py: - - - - - - - - - - results - - - - - - - - - - 275s test-recipe.py PASS (superficial) 276s autopkgtest [00:39:21]: @@@@@@@@@@@@@@@@@@@@ summary 276s test-recipe.py PASS (superficial) 291s Creating nova instance adt-noble-s390x-cpl-plugin-muse-20240419-003444-juju-7f2275-prod-proposed-migration-environment-3-da439567-7fe6-4862-95ea-6619021587c3 from image adt/ubuntu-noble-s390x-server-20240418.img (UUID 85e53509-ea4e-4742-afdb-a30c7e328507)...