0s autopkgtest [00:52:19]: starting date and time: 2024-04-19 00:52:19+0000 0s autopkgtest [00:52:19]: git checkout: 43bc6cdf gitlab-ci: do not include the salsa pipeline 0s autopkgtest [00:52:19]: host juju-7f2275-prod-proposed-migration-environment-2; command line: /home/ubuntu/autopkgtest/runner/autopkgtest --output-dir /tmp/autopkgtest-work.2o1pi_qj/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-fors --timeout-short=300 --timeout-copy=20000 --timeout-build=20000 --env=ADT_TEST_TRIGGERS=gsl/2.7.1+dfsg-6ubuntu2 -- ssh -s /home/ubuntu/autopkgtest/ssh-setup/nova -- --flavor autopkgtest --security-groups autopkgtest-juju-7f2275-prod-proposed-migration-environment-2@bos02-arm64-16.secgroup --name adt-noble-arm64-cpl-plugin-fors-20240419-005219-juju-7f2275-prod-proposed-migration-environment-2-e7495478-db50-4826-bd1b-53dcb506d97d --image adt/ubuntu-noble-arm64-server --keyname testbed-juju-7f2275-prod-proposed-migration-environment-2 --net-id=net_prod-proposed-migration -e TERM=linux -e ''"'"'http_proxy=http://squid.internal:3128'"'"'' -e ''"'"'https_proxy=http://squid.internal:3128'"'"'' -e ''"'"'no_proxy=127.0.0.1,127.0.1.1,login.ubuntu.com,localhost,localdomain,novalocal,internal,archive.ubuntu.com,ports.ubuntu.com,security.ubuntu.com,ddebs.ubuntu.com,changelogs.ubuntu.com,launchpadlibrarian.net,launchpadcontent.net,launchpad.net,10.24.0.0/24,keystone.ps5.canonical.com,objectstorage.prodstack5.canonical.com'"'"'' --mirror=http://ftpmaster.internal/ubuntu/ 112s autopkgtest [00:54:11]: testbed dpkg architecture: arm64 113s autopkgtest [00:54:12]: testbed apt version: 2.7.14build2 113s autopkgtest [00:54:12]: @@@@@@@@@@@@@@@@@@@@ test bed setup 114s Get:1 http://ftpmaster.internal/ubuntu noble-proposed InRelease [117 kB] 115s Get:2 http://ftpmaster.internal/ubuntu noble-proposed/restricted Sources [12.2 kB] 115s Get:3 http://ftpmaster.internal/ubuntu noble-proposed/multiverse Sources [2340 B] 115s Get:4 http://ftpmaster.internal/ubuntu noble-proposed/main Sources [54.2 kB] 115s Get:5 http://ftpmaster.internal/ubuntu noble-proposed/universe Sources [376 kB] 115s Get:6 http://ftpmaster.internal/ubuntu noble-proposed/main arm64 Packages [130 kB] 115s Get:7 http://ftpmaster.internal/ubuntu noble-proposed/main arm64 c-n-f Metadata [3144 B] 115s Get:8 http://ftpmaster.internal/ubuntu noble-proposed/restricted arm64 Packages [92.9 kB] 115s Get:9 http://ftpmaster.internal/ubuntu noble-proposed/restricted arm64 c-n-f Metadata [116 B] 115s Get:10 http://ftpmaster.internal/ubuntu noble-proposed/universe arm64 Packages [563 kB] 115s Get:11 http://ftpmaster.internal/ubuntu noble-proposed/universe arm64 c-n-f Metadata [8528 B] 115s Get:12 http://ftpmaster.internal/ubuntu noble-proposed/multiverse arm64 c-n-f Metadata [116 B] 119s Fetched 1360 kB in 2s (878 kB/s) 119s Reading package lists... 121s sh: 4: dhclient: not found 122s Reading package lists... 123s Building dependency tree... 123s Reading state information... 123s Calculating upgrade... 124s The following packages will be upgraded: 124s apport apport-core-dump-handler libkeyutils1 libnuma1 libunwind8 make man-db 124s netcat-openbsd numactl python3-apport python3-problem-report 124s 11 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 124s Need to get 1797 kB of archives. 124s After this operation, 1024 B of additional disk space will be used. 124s Get:1 http://ftpmaster.internal/ubuntu noble/main arm64 python3-problem-report all 2.28.1-0ubuntu1 [23.8 kB] 124s Get:2 http://ftpmaster.internal/ubuntu noble/main arm64 python3-apport all 2.28.1-0ubuntu1 [92.1 kB] 124s Get:3 http://ftpmaster.internal/ubuntu noble/main arm64 apport-core-dump-handler all 2.28.1-0ubuntu1 [16.8 kB] 124s Get:4 http://ftpmaster.internal/ubuntu noble/main arm64 apport all 2.28.1-0ubuntu1 [83.5 kB] 124s Get:5 http://ftpmaster.internal/ubuntu noble/main arm64 libkeyutils1 arm64 1.6.3-3build1 [9654 B] 124s Get:6 http://ftpmaster.internal/ubuntu noble/main arm64 netcat-openbsd arm64 1.226-1ubuntu2 [43.8 kB] 124s Get:7 http://ftpmaster.internal/ubuntu noble/main arm64 libnuma1 arm64 2.0.18-1build1 [23.6 kB] 124s Get:8 http://ftpmaster.internal/ubuntu noble/main arm64 man-db arm64 2.12.0-4build2 [1232 kB] 125s Get:9 http://ftpmaster.internal/ubuntu noble/main arm64 libunwind8 arm64 1.6.2-3build1 [53.5 kB] 125s Get:10 http://ftpmaster.internal/ubuntu noble/main arm64 make arm64 4.3-4.1build2 [178 kB] 125s Get:11 http://ftpmaster.internal/ubuntu noble/main arm64 numactl arm64 2.0.18-1build1 [39.5 kB] 125s Preconfiguring packages ... 125s Fetched 1797 kB in 1s (2557 kB/s) 126s (Reading database ... (Reading database ... 5% (Reading database ... 10% (Reading database ... 15% (Reading database ... 20% (Reading database ... 25% (Reading database ... 30% (Reading database ... 35% (Reading database ... 40% (Reading database ... 45% (Reading database ... 50% (Reading database ... 55% (Reading database ... 60% (Reading database ... 65% (Reading database ... 70% (Reading database ... 75% (Reading database ... 80% (Reading database ... 85% (Reading database ... 90% (Reading database ... 95% (Reading database ... 100% (Reading database ... 77740 files and directories currently installed.) 126s Preparing to unpack .../00-python3-problem-report_2.28.1-0ubuntu1_all.deb ... 126s Unpacking python3-problem-report (2.28.1-0ubuntu1) over (2.28.0-0ubuntu1) ... 126s Preparing to unpack .../01-python3-apport_2.28.1-0ubuntu1_all.deb ... 126s Unpacking python3-apport (2.28.1-0ubuntu1) over (2.28.0-0ubuntu1) ... 126s Preparing to unpack .../02-apport-core-dump-handler_2.28.1-0ubuntu1_all.deb ... 126s Unpacking apport-core-dump-handler (2.28.1-0ubuntu1) over (2.28.0-0ubuntu1) ... 126s Preparing to unpack .../03-apport_2.28.1-0ubuntu1_all.deb ... 126s Unpacking apport (2.28.1-0ubuntu1) over (2.28.0-0ubuntu1) ... 126s Preparing to unpack .../04-libkeyutils1_1.6.3-3build1_arm64.deb ... 126s Unpacking libkeyutils1:arm64 (1.6.3-3build1) over (1.6.3-3) ... 127s Preparing to unpack .../05-netcat-openbsd_1.226-1ubuntu2_arm64.deb ... 127s Unpacking netcat-openbsd (1.226-1ubuntu2) over (1.226-1ubuntu1) ... 127s Preparing to unpack .../06-libnuma1_2.0.18-1build1_arm64.deb ... 127s Unpacking libnuma1:arm64 (2.0.18-1build1) over (2.0.18-1) ... 127s Preparing to unpack .../07-man-db_2.12.0-4build2_arm64.deb ... 127s Unpacking man-db (2.12.0-4build2) over (2.12.0-4build1) ... 127s Preparing to unpack .../08-libunwind8_1.6.2-3build1_arm64.deb ... 127s Unpacking libunwind8:arm64 (1.6.2-3build1) over (1.6.2-3) ... 127s Preparing to unpack .../09-make_4.3-4.1build2_arm64.deb ... 127s Unpacking make (4.3-4.1build2) over (4.3-4.1build1) ... 127s Preparing to unpack .../10-numactl_2.0.18-1build1_arm64.deb ... 127s Unpacking numactl (2.0.18-1build1) over (2.0.18-1) ... 127s Setting up libkeyutils1:arm64 (1.6.3-3build1) ... 127s Setting up python3-problem-report (2.28.1-0ubuntu1) ... 128s Setting up netcat-openbsd (1.226-1ubuntu2) ... 128s Setting up man-db (2.12.0-4build2) ... 128s Updating database of manual pages ... 131s man-db.service is a disabled or a static unit not running, not starting it. 131s Setting up libunwind8:arm64 (1.6.2-3build1) ... 131s Setting up python3-apport (2.28.1-0ubuntu1) ... 132s Setting up make (4.3-4.1build2) ... 132s Setting up libnuma1:arm64 (2.0.18-1build1) ... 132s Setting up numactl (2.0.18-1build1) ... 132s Setting up apport-core-dump-handler (2.28.1-0ubuntu1) ... 135s Setting up apport (2.28.1-0ubuntu1) ... 135s Installing new version of config file /etc/apport/crashdb.conf ... 136s apport-autoreport.service is a disabled or a static unit not running, not starting it. 137s Processing triggers for libc-bin (2.39-0ubuntu8) ... 137s Reading package lists... 137s Building dependency tree... 137s Reading state information... 138s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 139s Hit:1 http://ftpmaster.internal/ubuntu noble-proposed InRelease 139s Hit:2 http://ftpmaster.internal/ubuntu noble InRelease 139s Hit:3 http://ftpmaster.internal/ubuntu noble-updates InRelease 139s Hit:4 http://ftpmaster.internal/ubuntu noble-security InRelease 142s Reading package lists... 142s Reading package lists... 143s Building dependency tree... 143s Reading state information... 143s Calculating upgrade... 144s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 144s Reading package lists... 144s Building dependency tree... 144s Reading state information... 145s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 146s autopkgtest [00:54:45]: rebooting testbed after setup commands that affected boot 302s autopkgtest [00:57:21]: testbed running kernel: Linux 6.8.0-22-generic #22-Ubuntu SMP PREEMPT_DYNAMIC Fri Apr 5 02:52:09 UTC 2024 306s autopkgtest [00:57:25]: @@@@@@@@@@@@@@@@@@@@ apt-source cpl-plugin-fors 310s Get:1 http://ftpmaster.internal/ubuntu noble/universe cpl-plugin-fors 5.5.7+dfsg-2build1 (dsc) [2571 B] 310s Get:2 http://ftpmaster.internal/ubuntu noble/universe cpl-plugin-fors 5.5.7+dfsg-2build1 (tar) [1299 kB] 310s Get:3 http://ftpmaster.internal/ubuntu noble/universe cpl-plugin-fors 5.5.7+dfsg-2build1 (diff) [13.3 kB] 310s gpgv: Signature made Tue Dec 7 17:25:56 2021 UTC 310s gpgv: using RSA key AC483F68DE728F43F2202FCA568D30F321B2133D 310s gpgv: issuer "steve.langasek@ubuntu.com" 310s gpgv: Can't check signature: No public key 310s dpkg-source: warning: cannot verify inline signature for ./cpl-plugin-fors_5.5.7+dfsg-2build1.dsc: no acceptable signature found 311s autopkgtest [00:57:30]: testing package cpl-plugin-fors version 5.5.7+dfsg-2build1 311s autopkgtest [00:57:30]: build not needed 343s autopkgtest [00:58:02]: test test-recipe.py: preparing testbed 344s Reading package lists... 345s Building dependency tree... 345s Reading state information... 345s Starting pkgProblemResolver with broken count: 0 346s Starting 2 pkgProblemResolver with broken count: 0 346s Done 346s The following additional packages will be installed: 346s cpl-plugin-fors libblas3 libcext0 libcfitsio10t64 libcplcore26 libcpldfs26 346s libcpldrs26 libcplui26 liberfa1 libfftw3-double3 libfftw3-single3 346s libgfortran5 libgomp1 libgsl27 libgslcblas0 libjs-jquery 346s libjs-jquery-hotkeys libjs-jquery-isonscreen libjs-jquery-metadata 346s libjs-jquery-tablesorter libjs-jquery-throttle-debounce libjs-sphinxdoc 346s libjs-underscore liblapack3 libwcs8 python3-astropy 346s python3-astropy-iers-data python3-coverage python3-cpl python3-dateutil 346s python3-erfa python3-hypothesis python3-iniconfig python3-numpy 346s python3-packaging python3-pluggy python3-ply python3-pytest 346s python3-pytest-arraydiff python3-pytest-astropy 346s python3-pytest-astropy-header python3-pytest-cov python3-pytest-doctestplus 346s python3-pytest-filter-subpackage python3-pytest-mock 346s python3-pytest-remotedata python3-sortedcontainers 346s Suggested packages: 347s cpl-plugin-fors-calib cpl-plugin-fors-doc libfftw3-bin libfftw3-dev 347s gsl-ref-psdoc | gsl-doc-pdf | gsl-doc-info | gsl-ref-html libxml2-utils 347s python-astropy-doc python3-astropy-affiliated python3-bs4 python3-h5py 347s python3-matplotlib python3-pandas python-coverage-doc gdb 347s python-hypothesis-doc gcc gfortran python3-dev python-ply-doc 347s python-pytest-mock-doc python-sortedcontainers-doc 347s Recommended packages: 347s source-extractor javascript-common libjs-jquery-datatables python3-scipy 347s python3-click 347s The following NEW packages will be installed: 347s autopkgtest-satdep cpl-plugin-fors libblas3 libcext0 libcfitsio10t64 347s libcplcore26 libcpldfs26 libcpldrs26 libcplui26 liberfa1 libfftw3-double3 347s libfftw3-single3 libgfortran5 libgomp1 libgsl27 libgslcblas0 libjs-jquery 347s libjs-jquery-hotkeys libjs-jquery-isonscreen libjs-jquery-metadata 347s libjs-jquery-tablesorter libjs-jquery-throttle-debounce libjs-sphinxdoc 347s libjs-underscore liblapack3 libwcs8 python3-astropy 347s python3-astropy-iers-data python3-coverage python3-cpl python3-dateutil 347s python3-erfa python3-hypothesis python3-iniconfig python3-numpy 347s python3-packaging python3-pluggy python3-ply python3-pytest 347s python3-pytest-arraydiff python3-pytest-astropy 347s python3-pytest-astropy-header python3-pytest-cov python3-pytest-doctestplus 347s python3-pytest-filter-subpackage python3-pytest-mock 347s python3-pytest-remotedata python3-sortedcontainers 347s 0 upgraded, 48 newly installed, 0 to remove and 0 not upgraded. 347s Need to get 18.9 MB/18.9 MB of archives. 347s After this operation, 89.6 MB of additional disk space will be used. 347s Get:1 /tmp/autopkgtest.hwRsl8/1-autopkgtest-satdep.deb autopkgtest-satdep arm64 0 [724 B] 347s Get:2 http://ftpmaster.internal/ubuntu noble/main arm64 libjs-jquery all 3.6.1+dfsg+~3.5.14-1 [328 kB] 347s Get:3 http://ftpmaster.internal/ubuntu noble/universe arm64 libjs-jquery-hotkeys all 0~20130707+git2d51e3a9+dfsg-2ubuntu2 [11.5 kB] 347s Get:4 http://ftpmaster.internal/ubuntu noble/universe arm64 libcext0 arm64 7.3.2+ds-1build3 [31.6 kB] 347s Get:5 http://ftpmaster.internal/ubuntu noble/universe arm64 libcfitsio10t64 arm64 4.3.1-1.1build2 [520 kB] 348s Get:6 http://ftpmaster.internal/ubuntu noble/main arm64 libgomp1 arm64 14-20240412-0ubuntu1 [144 kB] 348s Get:7 http://ftpmaster.internal/ubuntu noble/main arm64 libfftw3-double3 arm64 3.3.10-1ubuntu3 [384 kB] 348s Get:8 http://ftpmaster.internal/ubuntu noble/main arm64 libfftw3-single3 arm64 3.3.10-1ubuntu3 [583 kB] 349s Get:9 http://ftpmaster.internal/ubuntu noble/universe arm64 libcplcore26 arm64 7.3.2+ds-1build3 [446 kB] 349s Get:10 http://ftpmaster.internal/ubuntu noble/universe arm64 libcplui26 arm64 7.3.2+ds-1build3 [36.5 kB] 349s Get:11 http://ftpmaster.internal/ubuntu noble/universe arm64 libcpldfs26 arm64 7.3.2+ds-1build3 [39.0 kB] 349s Get:12 http://ftpmaster.internal/ubuntu noble/universe arm64 libwcs8 arm64 8.2.2+ds-3build2 [253 kB] 349s Get:13 http://ftpmaster.internal/ubuntu noble/universe arm64 libcpldrs26 arm64 7.3.2+ds-1build3 [62.8 kB] 350s Get:14 http://ftpmaster.internal/ubuntu noble-proposed/universe arm64 libgslcblas0 arm64 2.7.1+dfsg-6ubuntu2 [72.8 kB] 350s Get:15 http://ftpmaster.internal/ubuntu noble-proposed/universe arm64 libgsl27 arm64 2.7.1+dfsg-6ubuntu2 [918 kB] 350s Get:16 http://ftpmaster.internal/ubuntu noble/universe arm64 cpl-plugin-fors arm64 5.5.7+dfsg-2build1 [746 kB] 351s Get:17 http://ftpmaster.internal/ubuntu noble/main arm64 libblas3 arm64 3.12.0-3build1 [143 kB] 351s Get:18 http://ftpmaster.internal/ubuntu noble/main arm64 libgfortran5 arm64 14-20240412-0ubuntu1 [444 kB] 352s Get:19 http://ftpmaster.internal/ubuntu noble/universe arm64 libjs-jquery-metadata all 12-4 [6582 B] 352s Get:20 http://ftpmaster.internal/ubuntu noble/universe arm64 libjs-jquery-tablesorter all 1:2.31.3+dfsg1-3 [193 kB] 352s Get:21 http://ftpmaster.internal/ubuntu noble/universe arm64 libjs-jquery-throttle-debounce all 1.1+dfsg.1-2 [12.5 kB] 352s Get:22 http://ftpmaster.internal/ubuntu noble/main arm64 libjs-underscore all 1.13.4~dfsg+~1.11.4-3 [118 kB] 352s Get:23 http://ftpmaster.internal/ubuntu noble/main arm64 libjs-sphinxdoc all 7.2.6-6 [149 kB] 352s Get:24 http://ftpmaster.internal/ubuntu noble/main arm64 liblapack3 arm64 3.12.0-3build1 [2241 kB] 353s Get:25 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-iniconfig all 1.1.1-2 [6024 B] 353s Get:26 http://ftpmaster.internal/ubuntu noble/main arm64 python3-packaging all 24.0-1 [41.1 kB] 353s Get:27 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pluggy all 1.4.0-1 [20.4 kB] 353s Get:28 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pytest all 7.4.4-1 [305 kB] 354s Get:29 http://ftpmaster.internal/ubuntu noble/main arm64 python3-dateutil all 2.8.2-3ubuntu1 [79.4 kB] 354s Get:30 http://ftpmaster.internal/ubuntu noble/main arm64 python3-sortedcontainers all 2.4.0-2 [27.6 kB] 354s Get:31 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-hypothesis all 6.98.15-1 [311 kB] 354s Get:32 http://ftpmaster.internal/ubuntu noble/main arm64 python3-numpy arm64 1:1.26.4+ds-6ubuntu1 [3565 kB] 356s Get:33 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pytest-arraydiff all 0.6.1-2 [10.2 kB] 356s Get:34 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pytest-astropy-header all 0.2.2-1 [8190 B] 356s Get:35 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-coverage arm64 7.4.4+dfsg1-0ubuntu2 [148 kB] 356s Get:36 http://ftpmaster.internal/ubuntu noble/universe arm64 libjs-jquery-isonscreen all 1.2.0-1.1 [3244 B] 356s Get:37 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pytest-cov all 4.1.0-1 [21.5 kB] 356s Get:38 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pytest-doctestplus all 1.2.0-1 [23.1 kB] 356s Get:39 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pytest-filter-subpackage all 0.2.0-1 [6094 B] 356s Get:40 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pytest-mock all 3.12.0-1.1 [11.3 kB] 356s Get:41 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pytest-remotedata all 0.4.1-1 [8650 B] 356s Get:42 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-pytest-astropy all 0.11.0-1 [5902 B] 356s Get:43 http://ftpmaster.internal/ubuntu noble/main arm64 python3-ply all 3.11-6 [46.5 kB] 356s Get:44 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-astropy-iers-data all 0.2024.01.01.00.33.39-1 [2046 kB] 357s Get:45 http://ftpmaster.internal/ubuntu noble/universe arm64 liberfa1 arm64 2.0.1-1 [136 kB] 357s Get:46 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-erfa arm64 2.0.1.1+ds-3 [311 kB] 357s Get:47 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-astropy arm64 6.0.0-1ubuntu2 [3797 kB] 359s Get:48 http://ftpmaster.internal/ubuntu noble/universe arm64 python3-cpl arm64 0.7.4-2build10 [34.8 kB] 360s Fetched 18.9 MB in 13s (1481 kB/s) 360s Selecting previously unselected package libjs-jquery. 360s (Reading database ... (Reading database ... 5% (Reading database ... 10% (Reading database ... 15% (Reading database ... 20% (Reading database ... 25% (Reading database ... 30% (Reading database ... 35% (Reading database ... 40% (Reading database ... 45% (Reading database ... 50% (Reading database ... 55% (Reading database ... 60% (Reading database ... 65% (Reading database ... 70% (Reading database ... 75% (Reading database ... 80% (Reading database ... 85% (Reading database ... 90% (Reading database ... 95% (Reading database ... 100% (Reading database ... 77739 files and directories currently installed.) 360s Preparing to unpack .../00-libjs-jquery_3.6.1+dfsg+~3.5.14-1_all.deb ... 360s Unpacking libjs-jquery (3.6.1+dfsg+~3.5.14-1) ... 360s Selecting previously unselected package libjs-jquery-hotkeys. 360s Preparing to unpack .../01-libjs-jquery-hotkeys_0~20130707+git2d51e3a9+dfsg-2ubuntu2_all.deb ... 360s Unpacking libjs-jquery-hotkeys (0~20130707+git2d51e3a9+dfsg-2ubuntu2) ... 361s Selecting previously unselected package libcext0:arm64. 361s Preparing to unpack .../02-libcext0_7.3.2+ds-1build3_arm64.deb ... 361s Unpacking libcext0:arm64 (7.3.2+ds-1build3) ... 361s Selecting previously unselected package libcfitsio10t64:arm64. 361s Preparing to unpack .../03-libcfitsio10t64_4.3.1-1.1build2_arm64.deb ... 361s Unpacking libcfitsio10t64:arm64 (4.3.1-1.1build2) ... 361s Selecting previously unselected package libgomp1:arm64. 361s Preparing to unpack .../04-libgomp1_14-20240412-0ubuntu1_arm64.deb ... 361s Unpacking libgomp1:arm64 (14-20240412-0ubuntu1) ... 361s Selecting previously unselected package libfftw3-double3:arm64. 361s Preparing to unpack .../05-libfftw3-double3_3.3.10-1ubuntu3_arm64.deb ... 361s Unpacking libfftw3-double3:arm64 (3.3.10-1ubuntu3) ... 361s Selecting previously unselected package libfftw3-single3:arm64. 361s Preparing to unpack .../06-libfftw3-single3_3.3.10-1ubuntu3_arm64.deb ... 361s Unpacking libfftw3-single3:arm64 (3.3.10-1ubuntu3) ... 361s Selecting previously unselected package libcplcore26:arm64. 361s Preparing to unpack .../07-libcplcore26_7.3.2+ds-1build3_arm64.deb ... 361s Unpacking libcplcore26:arm64 (7.3.2+ds-1build3) ... 361s Selecting previously unselected package libcplui26:arm64. 361s Preparing to unpack .../08-libcplui26_7.3.2+ds-1build3_arm64.deb ... 361s Unpacking libcplui26:arm64 (7.3.2+ds-1build3) ... 361s Selecting previously unselected package libcpldfs26:arm64. 361s Preparing to unpack .../09-libcpldfs26_7.3.2+ds-1build3_arm64.deb ... 361s Unpacking libcpldfs26:arm64 (7.3.2+ds-1build3) ... 361s Selecting previously unselected package libwcs8:arm64. 361s Preparing to unpack .../10-libwcs8_8.2.2+ds-3build2_arm64.deb ... 361s Unpacking libwcs8:arm64 (8.2.2+ds-3build2) ... 361s Selecting previously unselected package libcpldrs26:arm64. 361s Preparing to unpack .../11-libcpldrs26_7.3.2+ds-1build3_arm64.deb ... 361s Unpacking libcpldrs26:arm64 (7.3.2+ds-1build3) ... 361s Selecting previously unselected package libgslcblas0:arm64. 361s Preparing to unpack .../12-libgslcblas0_2.7.1+dfsg-6ubuntu2_arm64.deb ... 361s Unpacking libgslcblas0:arm64 (2.7.1+dfsg-6ubuntu2) ... 361s Selecting previously unselected package libgsl27:arm64. 361s Preparing to unpack .../13-libgsl27_2.7.1+dfsg-6ubuntu2_arm64.deb ... 361s Unpacking libgsl27:arm64 (2.7.1+dfsg-6ubuntu2) ... 361s Selecting previously unselected package cpl-plugin-fors:arm64. 361s Preparing to unpack .../14-cpl-plugin-fors_5.5.7+dfsg-2build1_arm64.deb ... 361s Unpacking cpl-plugin-fors:arm64 (5.5.7+dfsg-2build1) ... 362s Selecting previously unselected package libblas3:arm64. 362s Preparing to unpack .../15-libblas3_3.12.0-3build1_arm64.deb ... 362s Unpacking libblas3:arm64 (3.12.0-3build1) ... 362s Selecting previously unselected package libgfortran5:arm64. 362s Preparing to unpack .../16-libgfortran5_14-20240412-0ubuntu1_arm64.deb ... 362s Unpacking libgfortran5:arm64 (14-20240412-0ubuntu1) ... 362s Selecting previously unselected package 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(0.7.4-2build10) ... 384s Setting up autopkgtest-satdep (0) ... 384s Processing triggers for man-db (2.12.0-4build2) ... 385s Processing triggers for libc-bin (2.39-0ubuntu8) ... 391s (Reading database ... 81662 files and directories currently installed.) 391s Removing autopkgtest-satdep (0) ... 392s autopkgtest [00:58:51]: test test-recipe.py: [----------------------- 393s Recipe fors_config: 393s version 5.5.7 393s Parameters: {'dispersion': 0.0, 'peakdetection': 250.0, 'wdegree': 4, 'cdegree': 4, 'startwavelength': 0.0, 'endwavelength': 0.0, 'instrument': '0', 'grism': '0', 'grism_id': '0', 'filter': '0', 'filter_id': '0'} 393s Docstring: Creation of FORS recipes configuration tables 393s 393s This recipe is used to create the so-called GRISM_TABLE, containing 393s all the FORS spectral pipeline configuration parameters related to a 393s specific grism. This is a way to provide for each specific instrument 393s mode a set of appropriate defaults for the recipe parameters. The 393s values assigned to each input parameter of fors_config are simply 393s copied to a FITS table consisting of one row, and as many columns as 393s the input parameter: each column will have the same name and type of 393s each parameter. Only the three parameters "instrument", "grism", and 393s "id" are not written to the table columns, but to the descriptor 393s header keywords INSTRUME, ESO INS GRIS1 NAME, and ESO INS GRIS1 ID, 393s that will be used by the automatic pipeline for appropriate data 393s association. Input files: none DO category: Type: 393s Explanation: Required: Output files: DO category: 393s Data type: Explanation: GRISM_TABLE FITS table 393s Recipe configuration parameters 393s 393s Parameters: 393s dispersion: Expected spectral dispersion (Angstrom/pixel) 393s (float; default: 0.0) 393s peakdetection: Peak detection threshold (ADU) (float; default: 393s 250.0) 393s wdegree: Degree of wavelength calibration polynomial (int; 393s default: 4) 393s cdegree: Degree of spectral curvature polynomial (int; 393s default: 4) 393s startwavelength: Start wavelength in spectral extraction (float; 393s default: 0.0) 393s endwavelength: End wavelength in spectral extraction (float; 393s default: 0.0) 393s instrument: Name of instrument (str; default: '0') 393s grism: Name of grism (str; default: '0') 393s grism_id: Grism ID (str; default: '0') 393s filter: Name of filter (str; default: '0') 393s filter_id: Filter ID (str; default: '0') 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_pmos_science: 393s version 5.5.7 393s Parameters: {'dispersion': 0.0, 'rebin': 1, 'skyalign': 0, 'wcolumn': 'WLEN', 'startwavelength': 0.0, 'endwavelength': 0.0, 'flux': True, 'flatfield': True, 'skymedian': False, 'skylocal': True, 'cosmics': False, 'slit_margin': 3, 'ext_radius': 12, 'cont_radius': 0, 'ext_mode': 1, 'match_tolerance': 5.0, 'time_normalise': True, 'chromatism': True, 'wollaston': True, 'qc': True} 393s Docstring: Extraction of scientific spectra 393s 393s This recipe is used to reduce scientific spectra using the extraction 393s mask and the products created by the recipe fors_mpol_calib. The 393s spectra are bias subtracted, flat fielded (if a normalised flat field 393s is specified) and remapped eliminating the optical distortions. The 393s wavelength calibration can be optionally upgraded using a number of 393s sky lines: if no sky lines catalog of wavelengths is specified, an 393s internal one is used instead. If the alignment to the sky lines is 393s performed, the input dispersion coefficients table is upgraded and 393s saved to disk, and a new CCD wavelengths map is created. This recipe 393s accepts both FORS1 and FORS2 frames. A grism table (typically 393s depending on the instrument mode, and in particular on the grism used) 393s may also be specified: this table contains a default recipe parameter 393s setting to control the way spectra are extracted for a specific 393s instrument mode, as it is used for automatic run of the pipeline on 393s Paranal and in Garching. If this table is specified, it will modify 393s the default recipe parameter setting, with the exception of those 393s parameters which have been explicitly modifyed on the command line. If 393s a grism table is not specified, the input recipe parameters values 393s will always be read from the command line, or from an esorex 393s configuration file if present, or from their generic default values 393s (that are rarely meaningful). Either a scientific or a standard star 393s exposure can be specified in input. The acronym SCI on products should 393s be read STD in case of standard stars observations. Input files: 393s DO category: Type: Explanation: 393s Required: SCIENCE_PMOS Raw Scientific 393s exposure Y or STANDARD_PMOS Raw Standard 393s star exposure Y MASTER_BIAS Calib Master 393s bias Y GRISM_TABLE Calib Grism 393s table . MASTER_SKYLINECAT Calib Sky 393s lines catalog . MASTER_NORM_FLAT_PMOS Calib 393s Normalised flat field . DISP_COEFF_PMOS Calib 393s Inverse dispersion Y CURV_COEFF_PMOS Calib 393s Spectral curvature Y SLIT_LOCATION_PMOS Calib 393s Slits positions table Y RETARDER_WAVEPLATE_CHROMATISM Calib 393s Chromatism correction . STD_PMOS_TABLE Calib 393s Linear pol. of std stars . Output files: DO category: 393s Data type: Explanation: REDUCED_SCI_PMOS FITS image 393s Extracted scientific spectra REDUCED_SKY_SCI_PMOS FITS image 393s Extracted sky spectra REDUCED_ERROR_SCI_PMOS FITS image 393s Errors on extracted spectra REDUCED_X_SCI_PMOS FITS image 393s X Stokes parameter (and L) REDUCED_ERROR_X_SCI_PMOS FITS image 393s Error on X Stokes parameter REDUCED_NUL_X_SCI_PMOS FITS image 393s Null parameter for X REDUCED_ANGLE_SCI_PMOS FITS image 393s Direction of linear polarization REDUCED_ERROR_ANGLE_SCI_PMOS FITS 393s image Error on polarization direction UNMAPPED_SCI_PMOS 393s FITS image Sky subtracted scientific spectra MAPPED_SCI_PMOS 393s FITS image Rectified scientific spectra MAPPED_ALL_SCI_PMOS 393s FITS image Rectified science spectra with sky MAPPED_SKY_SCI_PMOS 393s FITS image Rectified sky spectra UNMAPPED_SKY_SCI_PMOS FITS 393s image Sky on CCD OBJECT_TABLE_SCI_PMOS FITS table Positions 393s of detected objects OBJECT_TABLE_POL_SCI_PMOS FITS table 393s Positions of real objects Only if the sky-alignment of the 393s wavelength solution is requested: DISP_COEFF_SCI_PMOS FITS 393s table Upgraded dispersion coefficients WAVELENGTH_MAP_SCI_PMOS 393s FITS image Upgraded wavelength map 393s 393s Parameters: 393s dispersion: Expected spectral dispersion (Angstrom/pixel) 393s (float; default: 0.0) 393s rebin: Rebin (pixel) (int; default: 1) 393s skyalign: Polynomial order for sky lines alignment, or -1 to 393s avoid alignment (int; default: 0) 393s wcolumn: Name of sky line catalog table column with 393s wavelengths (str; default: 'WLEN') 393s startwavelength: Start wavelength in spectral extraction (float; 393s default: 0.0) 393s endwavelength: End wavelength in spectral extraction (float; 393s default: 0.0) 393s flux: Apply flux conservation (bool; default: True) 393s flatfield: Apply flat field (bool; default: True) 393s skymedian: Sky subtraction from extracted slit spectra (bool; 393s default: False) 393s skylocal: Sky subtraction from CCD slit spectra (bool; 393s default: True) 393s cosmics: Eliminate cosmic rays hits (only if local sky 393s subtraction is also requested) (bool; default: 393s False) 393s slit_margin: Number of pixels to exclude at each slit in object 393s detection and extraction (int; default: 3) 393s ext_radius: Maximum extraction radius for detected objects 393s (pixel) (int; default: 12) 393s cont_radius: Minimum distance at which two objects of equal 393s luminosity do not contaminate each other (pixel) 393s (int; default: 0) 393s ext_mode: Object extraction method: 0 = aperture, 1 = Horne 393s optimal extraction (int; default: 1) 393s match_tolerance: Tolerance for matching spectra from the same object 393s at different angles and beams (pixel) (float; 393s default: 5.0) 393s time_normalise: Normalise output spectra by the exposure time (bool; 393s default: True) 393s chromatism: Chromatism correction to polarization angles (bool; 393s default: True) 393s wollaston: Wollaston mounting (FORS2 only): true = 0 degrees 393s (ord. beam on top, extr. beam on bottom), false = 393s 180 degrees (beams are reversed), for FORS1 is 393s frozen to true (bool; default: True) 393s qc: Compute QC1 parameters (bool; default: True) 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_detect_spectra: 393s version 5.5.7 393s Parameters: {'dispersion': 0.0, 'peakdetection': 0.0, 'wdegree': 0, 'wradius': 4, 'wreject': 0.7, 'wcolumn': 'WLEN', 'startwavelength': 0.0, 'endwavelength': 0.0, 'slit_ident': True} 393s Docstring: Detect MOS/MXU spectra on CCD 393s 393s This recipe is used to detect and locate MOS/MXU slit spectra on the 393s CCD, applying a pattern-matching algorithm. The input spectral 393s exposure must contain spectra with the dispersion direction 393s approximately horizontal, with blue on the left and red on the right. 393s Use recipe fors_wave_calib_lss for LSS data, or for MOS/MXU data where 393s all slits have the same offset. The rows of the input spectral 393s exposure are processed separately, one by one. First, the background 393s continuum is removed. Second, a list of positions of reference lines 393s candidates is created. Only peaks above a given threshold (specified 393s by the parameter --peakdetection) are selected. Third, the pattern- 393s matching task selects from the found peaks the ones corresponding to 393s the reference lines, listed in the input line catalog, associating 393s them to the appropriate wavelengths. The ensuing polynomial fit is 393s used to locate the central wavelength of the applied grism along each 393s image row. The contributions from all rows form an image of the 393s location of all spectra, that can be used as a starting point for the 393s proper modeling of the optical and spectral distortions. For more 393s details on this reduction strategy please refer to the FORS Pipeline 393s User's Manual. Note that specifying an input GRISM_TABLE will set 393s some of the recipe configuration parameters to default values valid 393s for a particular grism. Again, see the pipeline manual for more 393s details. In the table below the MXU acronym can be alternatively read 393s as MOS. Input files: DO category: Type: 393s Explanation: Required: LAMP_UNBIAS_MXU Calib 393s Bias subtracted arc Y MASTER_LINECAT Calib 393s Line catalog Y GRISM_TABLE Calib 393s Grism table . Output files: DO category: 393s Data type: Explanation: SLIT_MAP_MXU FITS image Map 393s of central wavelength on CCD SLIT_LOCATION_DETECT_MXU FITS table 393s Slits positions on CCD SPECTRA_DETECTION_MXU FITS image Check 393s of preliminary detection 393s 393s Parameters: 393s dispersion: Expected spectral dispersion (Angstrom/pixel) 393s (float; default: 0.0) 393s peakdetection: Initial peak detection threshold (ADU) (float; 393s default: 0.0) 393s wdegree: Degree of wavelength calibration polynomial (int; 393s default: 0) 393s wradius: Search radius if iterating pattern-matching with 393s first-guess method (int; default: 4) 393s wreject: Rejection threshold in dispersion relation fit 393s (pixel) (float; default: 0.7) 393s wcolumn: Name of line catalog table column with wavelengths 393s (str; default: 'WLEN') 393s startwavelength: Start wavelength in spectral extraction (float; 393s default: 0.0) 393s endwavelength: End wavelength in spectral extraction (float; 393s default: 0.0) 393s slit_ident: Attempt slit identification for MOS or MXU (bool; 393s default: True) 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_img_science: 393s version 5.5.7 393s Parameters: {'magsyserr': 0.01, 'sex_exe': '/usr/bin/source-extractor', 'sex_config': '/usr/share/cpl-plugins/fors-5.5.7/config/fors.sex', 'sex_mag': 'MAG_APER', 'sex_magerr': 'MAGERR_APER', 'sex_radius': 64, 'idp_generate': False, 'idp_weights_threshold': 0.5} 393s Docstring: Reduce imaging scientific exposure 393s 393s Input files: DO category: Type: Explanation: 393s Number: SCIENCE_IMG Raw Science image 393s 1 MASTER_BIAS FITS image Master bias 393s 1 MASTER_SKY_FLAT_IMG FITS image Master sky flat field 393s 1 PHOT_COEFF_TABLE FITS table Observed extinction 393s coefficients 0+ EXTINCTION_PER_NIGHT FITS table 393s Extinction per night 0+ 393s STATIC_PHOT_COEFF_TABLE FITS table Static filters photometry 393s coefficients 0+ DETECTOR_ILLUMINATED_REGION FITS table 393s Table with detector illuminated regions 0+ Output files: DO 393s category: Data type: Explanation: SCIENCE_REDUCED_IMG 393s FITS image Reduced science image PHOT_BACKGROUND_SCI_IMG FITS 393s image Reduced science image background SOURCES_SCI_IMG 393s FITS image Unfiltered SExtractor output OBJECT_TABLE_SCI_IMG 393s FITS table Extracted sources properties SCIENCE_REDUCED_IMG_IDP 393s FITS image Reduced science image in IDP-compliant format 393s SCIENCE_REDUCED_WEIGHT_IDP FITS image Ancillary file with the weights 393s for IDP the image SCIENCE_REDUCED_ERR_IDP FITS image Ancillary 393s file with the errors for IDP the image 393s 393s Parameters: 393s magsyserr: Systematic error in magnitude (float; default: 393s 0.01) 393s sex_exe: SExtractor executable (str; default: 393s '/usr/bin/source-extractor') 393s sex_config: SExtractor configuration file (str; default: 393s '/usr/share/cpl- 393s plugins/fors-5.5.7/config/fors.sex') 393s sex_mag: SExtractor magnitude (str; default: 393s 'MAG_APER') 393s sex_magerr: SExtractor magnitude error (str; default: 393s 'MAGERR_APER') 393s sex_radius: Background error map median filter radius 393s (unbinned pixels) (int; default: 64) 393s idp_generate: If TRUE compliant IDP science products are 393s generated (bool; default: False) 393s idp_weights_threshold: Every pixel in the MASTER_SKY_FLAT_IMG below 393s the threshold will be put to 0 in the weight- 393s map, 1 otherwise. Ignored if IDP generation is 393s not requested (float; default: 0.5) 393s Author: ESO PPS Group 393s 393s 393s Recipe fors_normalise_flat: 393s version 5.5.7 393s Parameters: {'dispersion': 0.0, 'startwavelength': 0.0, 'endwavelength': 0.0, 'spa_polydegree': -1, 'sradius': 10, 'disp_nknots': -1, 'dradius': 10, 'dradius_aver': 10, 'splfit_threshold': 0.01} 393s Docstring: Normalise master flat spectrum 393s 393s This recipe is used to normalise a master flat field frame dividing it 393s by its large scale illumination trend. This recipe can be applied both 393s to generic multi-slit (MOS/MXU) and to long slit exposures (either 393s LSS, or LSS-like MOS/MXU), even if different normalisation methods are 393s applied in such different cases. The input master flat field image is 393s the product of the recipe fors_flat. The input spectral curvature 393s table, product of the recipe fors_detect_spectra, is only required in 393s the case of multi-slit data. In the case of multi-slit data, the flat 393s field spectra are spatially rectified, heavily smoothed, and then 393s mapped back on the CCD. Then the master flat image is divided by its 393s smoothed counterpart. The smoothing may be obtained either by applying 393s a running median filter of specified sizes, or by polynomial fitting 393s along the dispersion direction performed independently for each row of 393s the spatially remapped spectra. In the case of long-slit data, the 393s smoothing can still be obtained either by applying a running median 393s filter or by polynomial fitting, but the polynomial fitting will be 393s performed along the spatial direction, for each column of the 393s spectrum. In the table below the MXU acronym can be alternatively 393s read as MOS or LSS. Input files: DO category: Type: 393s Explanation: Required: MASTER_SCREEN_FLAT_MXU Calib 393s Master flat frame Y DISP_COEFF_MXU Calib 393s Wavelength calibration Y CURV_COEFF_MXU Calib 393s Spectral curvature . SLIT_LOCATION_MXU Calib 393s Slit detection . GRISM_TABLE Calib 393s Grism table Y Output files: DO category: 393s Data type: Explanation: MASTER_NORM_FLAT_MXU FITS image 393s Normalised flat field 393s 393s Parameters: 393s dispersion: Expected spectral dispersion (Angstrom/pixel) 393s (float; default: 0.0) 393s startwavelength: Start wavelength in spectral extraction (float; 393s default: 0.0) 393s endwavelength: End wavelength in spectral extraction (float; 393s default: 0.0) 393s spa_polydegree: Polynomial degree for the flat field fitting along 393s spatial direction (int; default: -1) 393s sradius: Smooth box radius for flat field along spatial 393s direction (int; default: 10) 393s disp_nknots: Number of knots in flat field fitting splines along 393s dispersion direction (int; default: -1) 393s dradius: Smooth box radius (median) for flat field along 393s dispersion direction (int; default: 10) 393s dradius_aver: Smooth box radius (average) for flat field along 393s dispersion direction (performed after median 393s smoothing) (int; default: 10) 393s splfit_threshold: Threshold percentage for flat spline fittingwith 393s respect to the maximum (float; default: 0.01) 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_calib: 393s version 5.5.7 393s Parameters: {'dispersion': 0.0, 'peakdetection': 0.0, 'wdegree': 0, 'wradius': 4, 'wreject': 0.7, 'wmode': 2, 'wmosmode': 0, 'ignore_lines': '', 'used_linesets': 'standard', 'cdegree': -1, 'cmode': 1, 'startwavelength': 0.0, 'endwavelength': 0.0, 'slit_ident': False, 'stack_method': 'sum', 'ksigma': '-3.0,3.0', 'kiter': 999, 's_degree': -1, 'sradius': -1, 'd_nknots': -1, 'dradius': 10, 'dradius_aver': -1, 'fit_threshold': 0.01, 'nonlinear_level': 60000.0, 'max_nonlinear_ratio': 0.2} 393s Docstring: Determination of the extraction mask 393s 393s This recipe is used to identify reference lines on LSS, MOS and MXU 393s arc lamp exposures, and trace the spectral edges on the corresponding 393s flat field exposures. This information is used to determine the 393s spectral extraction mask to be applied in the scientific data 393s reduction, performed with the recipe fors_science. This recipe accepts 393s both FORS1 and FORS2 frames. The input arc lamp and flat field 393s exposures are assumed to be obtained quasi-simultaneously, so that 393s they would be described by exactly the same instrument distortions. A 393s line catalog must be specified, containing the wavelengths of the 393s reference arc lamp lines used for the wavelength calibration. A grism 393s table (typically depending on the instrument mode, and in particular 393s on the grism used) may also be specified: this table contains a 393s default recipe parameter setting to control the way spectra are 393s extracted for a specific instrument mode, as it is used for automatic 393s run of the pipeline on Paranal and in Garching. If this table is 393s specified, it will modify the default recipe parameter setting, with 393s the exception of those parameters which have been explicitly modified 393s on the command line. If a grism table is not specified, the input 393s recipe parameters values will always be read from the command line, or 393s from an esorex configuration file if present, or from their generic 393s default values (that are rarely meaningful). Finally a master bias 393s frame must be input to this recipe. In the table below the MXU acronym 393s can be read alternatively as MOS and LSS, with the exception of 393s CURV_COEFF_LSS, CURV_TRACES_LSS, SPATIAL_MAP_LSS, 393s SPECTRA_DETECTION_LSS, and and SLIT_MAP_LSS, which are never created. 393s The products SPECTRA_DETECTION_MXU, SLIT_MAP_MXU, and 393s DISP_RESIDUALS_MXU, are just created if the --check parameter is set 393s to true. The product GLOBAL_DISTORTION_TABLE is just created if more 393s than 12 separate spectra are found in the CCD. Input files: DO 393s category: Type: Explanation: Required: 393s SCREEN_FLAT_MXU Raw Flat field exposures Y 393s LAMP_MXU Raw Arc lamp exposure Y 393s MASTER_BIAS Calib Master Bias frame Y 393s MASTER_LINECAT Calib Line catalog Y 393s GRISM_TABLE Calib Grism table . Output 393s files: DO category: Data type: Explanation: 393s MASTER_SCREEN_FLAT_MXU FITS image Combined (sum) flat field 393s MASTER_NORM_FLAT_MXU FITS image Normalised flat field 393s MAPPED_SCREEN_FLAT_MXU FITS image Wavelength calibrated flat field 393s MAPPED_NORM_FLAT_MXU FITS image Wavelength calibrated normalised 393s flat REDUCED_LAMP_MXU FITS image Wavelength calibrated arc 393s spectrum DISP_COEFF_MXU FITS table Inverse dispersion 393s coefficients DISP_RESIDUALS_MXU FITS image Residuals in 393s wavelength calibration DISP_RESIDUALS_TABLE_MXU FITS table 393s Residuals in wavelength calibration DELTA_IMAGE_MXU FITS 393s image Offset vs linear wavelength calib WAVELENGTH_MAP_MXU 393s FITS image Wavelength for each pixel on CCD SPECTRA_DETECTION_MXU 393s FITS image Check for preliminary detection SLIT_MAP_MXU 393s FITS image Map of central wavelength on CCD CURV_TRACES_MXU 393s FITS table Spectral curvature traces CURV_COEFF_MXU FITS 393s table Spectral curvature coefficients SPATIAL_MAP_MXU FITS 393s image Spatial position along slit on CCD SPECTRAL_RESOLUTION_MXU 393s FITS table Resolution at reference arc lines DETECTED_LINES_MXU 393s FITS table All the lines detected in the arc ARC_RECTIFIED_MXU 393s FITS image The spatial rectified arc SLIT_LOCATION_MXU FITS 393s table Slits on product frames and CCD GLOBAL_DISTORTION_TABLE FITS 393s table Global distortions table FLAT_SED_LSS FITS image 393s Average SED for each of the slitsi 393s 393s Parameters: 393s dispersion: Expected spectral dispersion (Angstrom/pixel) 393s (float; default: 0.0) 393s peakdetection: Initial peak detection threshold (ADU) (float; 393s default: 0.0) 393s wdegree: Degree of wavelength calibration polynomial 393s (int; default: 0) 393s wradius: Search radius if iterating pattern-matching with 393s first-guess method (int; default: 4) 393s wreject: Rejection threshold in dispersion relation fit 393s (pixel) (float; default: 0.7) 393s wmode: Interpolation mode of wavelength solution 393s applicable to LSS-like data (0 = no 393s interpolation, 1 = fill gaps, 2 = global model) 393s (int; default: 2) 393s wmosmode: Interpolation mode of wavelength solution (0 = 393s no interpolation, 1 = local (slit) solution, 2 = 393s global model) (int; default: 0) 393s ignore_lines: Catalog lines nearest to wavelengths in this 393s list will be ignored for wavelength calibration 393s (str; default: '') 393s used_linesets: Linesets to use. Valid are 'standard' 393s and'extended' (see column LINE_SET in the line 393s catalogue) (str; default: 'standard') 393s cdegree: Degree of spectral curvature polynomial (int; 393s default: -1) 393s cmode: Interpolation mode of curvature solution 393s applicable to MOS-like data (0 = no 393s interpolation, 1 = fill gaps, 2 = global model) 393s (int; default: 1) 393s startwavelength: Start wavelength in spectral extraction (float; 393s default: 0.0) 393s endwavelength: End wavelength in spectral extraction (float; 393s default: 0.0) 393s slit_ident: Attempt slit identification for MOS or MXU 393s (bool; default: False) 393s stack_method: Frames combination method (str; default: 'sum') 393s ksigma: Low and high threshold in ksigma method (str; 393s default: '-3.0,3.0') 393s kiter: Max number of iterations in ksigma method (int; 393s default: 999) 393s s_degree: Polynomial degree for the flat field fitting 393s along spatial direction (int; default: -1) 393s sradius: Smooth box radius for flat field along spatial 393s direction (int; default: -1) 393s d_nknots: Number of knots in flat field fitting splines 393s along dispersion direction (int; default: -1) 393s dradius: Smooth box radius (median) for flat field along 393s dispersion direction (int; default: 10) 393s dradius_aver: Smooth box radius (average) for flat field along 393s dispersion direction (performed after median 393s smoothing) (int; default: -1) 393s fit_threshold: Threshold percentage for flat spline fittingwith 393s respect to the maximum (float; default: 0.01) 393s nonlinear_level: Level above which the detector is not linear 393s (float; default: 60000.0) 393s max_nonlinear_ratio: Maximum allowed ratio of non-linear pixels per 393s slit (float; default: 0.2) 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_photometry: 393s version 5.5.7 393s Parameters: {'fitz': True, 'fit_all_mag': False, 'fite': 'pernight', 'fitc': False, 'use_all_stars': False, 'degreef1': 0, 'degreef2': -1, 'degreep': 0, 'mjd_obs_target': -1.0} 393s Docstring: Compute corrected flatfield 393s 393s Input files: DO category: Type: Explanation: 393s Number: PHOT_TABLE FITS table Expected extinction 393s params 1 ALIGNED_PHOT FITS table Photometry 393s 1+ MASTER_SKY_FLAT_IMG FITS image Master flat field 393s 1 Output files: DO category: Data type: Explanation: 393s PHOT_COEFF_TABLE FITS image Observed extinction 393s coefficients CORRECTION_MAP FITS image Correction map 393s (magnitude) CORRECTION_FACTOR FITS image Correction map 393s (flux) MASTER_FLAT_IMG FITS image Corrected master flat 393s field 393s 393s Parameters: 393s fitz: Fit zeropoint (bool; default: True) 393s fit_all_mag: Always fit star magnitudes (bool; default: False) 393s fite: Fit atmospheric extinctions (str; default: 393s 'pernight') 393s fitc: Fit color correction term (bool; default: False) 393s use_all_stars: Use also non-standard stars to fit polynomial f 393s (bool; default: False) 393s degreef1: FLatfield correction map polynomial degree (x) (int; 393s default: 0) 393s degreef2: Flatfield correction map polynomial degree (y), or 393s negative for triangular coefficient matrix (int; 393s default: -1) 393s degreep: Extinction/color coupling degree (int; default: 0) 393s mjd_obs_target: MJD-OBS used to match the raw frame from which 393s EXTINCTION_PER_NIGHT and PHOT_COEFF inherit MJD-OBS. 393s If negative theMJD-OBS of the first raw frame isused 393s (float; default: -1.0) 393s Author: Jonas M. Larsen 393s 393s 393s Recipe fors_wave_calib_lss: 393s version 5.5.7 393s Parameters: {'dispersion': 0.0, 'peakdetection': 0.0, 'wdegree': 0, 'wradius': 4, 'wreject': 0.7, 'wcolumn': 'WLEN', 'startwavelength': 0.0, 'endwavelength': 0.0, 'wmode': 2} 393s Docstring: Derive dispersion relation from long-slit arc lamp frame 393s 393s This recipe is used to wavelength calibrate one long slit spectrum, 393s i.e., a FORS spectral obtained either in LSS mode or in MOS/MXU mode 393s with all slits at the same offset. A pattern-matching algorithm is 393s applied as in recipe fors_detect_spectra. For more details on this 393s data reduction strategy please refer to the FORS Pipeline User's 393s Manual. Note that specifying an input GRISM_TABLE will set some of 393s the recipe configuration parameters to default values valid for a 393s particular grism. In the table below the LSS acronym can be 393s alternatively read as MOS or MXU. Input files: DO category: 393s Type: Explanation: Required: LAMP_UNBIAS_LSS 393s Calib Arc lamp exposure Y MASTER_LINECAT 393s Calib Line catalog Y GRISM_TABLE 393s Calib Grism table . Output files: DO category: 393s Data type: Explanation: REDUCED_LAMP_LSS FITS image 393s Calibrated arc lamp exposure DISP_COEFF_LSS FITS table 393s Inverse dispersion coefficients DISP_RESIDUALS_LSS FITS 393s image Image of modeling residuals WAVELENGTH_MAP_LSS FITS 393s image Wavelengths mapped on CCD SLIT_LOCATION_LSS FITS 393s image Background subtracted arc frame SPECTRAL_RESOLUTION_LSS 393s FITS table Spectral resolution table 393s 393s Parameters: 393s dispersion: Expected spectral dispersion (Angstrom/pixel) 393s (float; default: 0.0) 393s peakdetection: Initial peak detection threshold (ADU) (float; 393s default: 0.0) 393s wdegree: Degree of wavelength calibration polynomial (int; 393s default: 0) 393s wradius: Search radius if iterating pattern-matching with 393s first-guess method (int; default: 4) 393s wreject: Rejection threshold in dispersion relation fit 393s (pixel) (float; default: 0.7) 393s wcolumn: Name of line catalog table column with wavelengths 393s (str; default: 'WLEN') 393s startwavelength: Start wavelength in spectral extraction (float; 393s default: 0.0) 393s endwavelength: End wavelength in spectral extraction (float; 393s default: 0.0) 393s wmode: Interpolation mode of wavelength solution (0 = no 393s interpolation, 1 = fill gaps, 2 = global model) 393s (int; default: 2) 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_flatfield: 393s version 5.5.7 393s Parameters: {} 393s Docstring: Flat field correction of input frame 393s 393s This recipe is used to divide the input frame by the normalised flat 393s field frame produced by recipe fors_normalise_flat. The input frame 393s must be already bias subtracted (e.g., by recipe fors_remove_bias). In 393s the table below the MXU acronym can be alternatively read as MOS and 393s LSS. Input files: DO category: Type: 393s Explanation: Required: SCIENCE_UNBIAS_MXU or 393s STANDARD_UNBIAS_MXU Raw Bias subtracted frame Y 393s MASTER_NORM_FLAT_MXU Calib Normalised flat frame Y 393s Output files: DO category: Data type: Explanation: 393s SCIENCE_UNFLAT_MXU or STANDARD_UNFLAT_MXU FITS image Flat field 393s corrected frame 393s 393s No parameters 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_extract_slits: 393s version 5.5.7 393s Parameters: {'dispersion': 0.0, 'startwavelength': 0.0, 'endwavelength': 0.0, 'flux': True} 393s Docstring: Spatial rectification of spectral image 393s 393s This recipe is used to extract MOS/MXU slit spectra, following their 393s curvature, and to remap them into a spatially rectified image. Please 393s refer to the FORS Pipeline User's Manual for details about the spectra 393s remapping technique. Note however that the interpolation is done 393s exclusively along the spatial direction, and therefore the output 393s rectified image will have the same x size of the input spectral image. 393s In the table below the MXU acronym can be alternatively read as MOS. 393s Input files: DO category: Type: Explanation: 393s Required: LAMP_UNBIAS_MXU or SCIENCE_UNBIAS_MXU or 393s SCIENCE_UNFLAT_MXU or STANDARD_UNBIAS_MXU or STANDARD_UNFLAT_MXU 393s or UNMAPPED_SCI_MXU or UNMAPPED_STD_MXU or UNMAPPED_SKY_SCI_MXU 393s or UNMAPPED_SKY_STD_MXU Calib Spectral frame Y 393s SLIT_LOCATION_DETECT_MXU or SLIT_LOCATION_MXU Calib 393s Master flat frame Y CURV_COEFF_MXU Calib 393s Spectral curvature Y GRISM_TABLE Calib 393s Grism table . Output files: DO category: 393s Data type: Explanation: RECTIFIED_LAMP_MXU or 393s RECTIFIED_ALL_SCI_MXU or RECTIFIED_ALL_STD_MXU or 393s RECTIFIED_SCI_MXU or RECTIFIED_STD_MXU or RECTIFIED_SKY_SCI_MXU 393s or RECTIFIED_SKY_STD_MXU FITS image Rectified slit spectra 393s 393s Parameters: 393s dispersion: Expected spectral dispersion (Angstrom/pixel) 393s (float; default: 0.0) 393s startwavelength: Start wavelength in spectral extraction (float; 393s default: 0.0) 393s endwavelength: End wavelength in spectral extraction (float; 393s default: 0.0) 393s flux: Apply flux conservation (bool; default: True) 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_trace_flat: 393s version 5.5.7 393s Parameters: {'dispersion': 0.0, 'startwavelength': 0.0, 'endwavelength': 0.0, 'cdegree': 0, 'cmode': 1} 393s Docstring: Determine spectral curvature model 393s 393s This recipe is used to trace the edges of MOS/MXU flat field slit 393s spectra and determine the spectral curvature solution. The input 393s master flat field image, product of the recipe fors_flat, is expected 393s to be oriented with horizontal dispersion direction and red 393s wavelengths on the right side. The input slits location table should 393s be the product of the recipe fors_detect_spectra. The input master 393s flat image is shifted one pixel down and is subtracted from the 393s original image. The result is a vertical gradient map. Next, the 393s negative values are forced positive, to obtain an absolute gradient 393s map. The map is passed with a horizontal median filter, and after that 393s the gradient peaks are traced starting from the slits positions listed 393s in the input slits location table. The number of pixels to the left 393s and to the right of the reference pixel is trivially derived from the 393s specified spectral range and spectral dispersion. The output spectral 393s curvature table contains the coefficients of the polynomial fitting of 393s the found traces, while the output trace table contains the traced 393s spectral edges positions in CCD (Y) coordinates for each spectrum, and 393s their comparison with their modeling. A spatial map is also created, 393s where to each CCD pixel is assigned the value of the spatial 393s coordinate along the slit (in pixel). For more details please refer to 393s the FORS Pipeline User's Manual. Note that specifying an input 393s GRISM_TABLE will set some of the recipe configuration parameters to 393s default values valid for a particular grism. Again, see the pipeline 393s manual for more details. In the table below the MXU acronym can be 393s alternatively read as MOS. Input files: DO category: 393s Type: Explanation: Required: MASTER_SCREEN_FLAT_MXU 393s Calib Master flat frame Y SLIT_LOCATION_DETECT_MXU 393s Calib Slits location Y GRISM_TABLE 393s Calib Grism table . Output files: DO category: 393s Data type: Explanation: CURV_TRACES_MXU FITS table Flat 393s field tracings CURV_COEFF_MXU FITS table Spectral 393s curvature table SPATIAL_MAP_MXU FITS image Map of 393s spatial coordinate 393s 393s Parameters: 393s dispersion: Expected spectral dispersion (Angstrom/pixel) 393s (float; default: 0.0) 393s startwavelength: Start wavelength in spectral extraction (float; 393s default: 0.0) 393s endwavelength: End wavelength in spectral extraction (float; 393s default: 0.0) 393s cdegree: Degree of spectral curvature polynomial (int; 393s default: 0) 393s cmode: Interpolation mode of curvature solution applicable 393s to MOS-like data (0 = no interpolation, 1 = fill 393s gaps, 2 = global model) (int; default: 1) 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_align_sky_lss: 393s version 5.5.7 393s Parameters: {'dispersion': 0.0, 'startwavelength': 0.0, 'endwavelength': 0.0, 'skyalign': 0, 'wcolumn': 'WLEN'} 393s Docstring: Upgrade wavelength solution using sky lines 393s 393s This recipe is used to align the wavelength solution based on the arc 393s lamp exposure on a set of sky lines observed on a scientific exposure. 393s The input scientific frames are produced by the recipes 393s fors_remove_bias and fors_flatfield. An input catalog of sky lines can 393s be specified, or an internal one is used. This recipe should be 393s applied to LSS or long-slit like data (MOS/MXU with all slits at the 393s same offset). For multi-slit MOS/MXU data use recipe fors_align_sky 393s instead. Please refer to the FORS PIpeline User's Manual for more 393s details. In the table below the MXU acronym can be alternatively read 393s as MOS and LSS, and SCI as STD. Input files: DO category: 393s Type: Explanation: Required: SCIENCE_UNBIAS_MXU or 393s SCIENCE_UNFLAT_MXU or STANDARD_UNBIAS_MXU or STANDARD_UNFLAT_MXU 393s Calib Frame with sky lines Y DISP_COEFF_MXU 393s Calib Dispersion solution Y SLIT_LOCATION_MXU 393s Calib Slit location on CCD Y MASTER_SKYLINECAT 393s Calib Catalog of sky lines . GRISM_TABLE 393s Calib Grism table . Output files: DO category: 393s Data type: Explanation: SKY_SHIFTS_LONG_SCI_MXU FITS table 393s Observed sky lines offsets WAVELENGTH_MAP_SCI_MXU FITS image 393s Wavelength mapped on CCD DISP_COEFF_SCI_MXU FITS image 393s Upgraded dispersion solution 393s 393s Parameters: 393s dispersion: Expected spectral dispersion (Angstrom/pixel) 393s (float; default: 0.0) 393s startwavelength: Start wavelength in spectral extraction (float; 393s default: 0.0) 393s endwavelength: End wavelength in spectral extraction (float; 393s default: 0.0) 393s skyalign: Polynomial order for sky lines alignment (int; 393s default: 0) 393s wcolumn: Name of sky line catalog table column with 393s wavelengths (str; default: 'WLEN') 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_wave_calib: 393s version 5.5.7 393s Parameters: {'dispersion': 0.0, 'peakdetection': 0.0, 'wdegree': 0, 'wradius': 4, 'wreject': 0.7, 'wcolumn': 'WLEN', 'startwavelength': 0.0, 'endwavelength': 0.0} 393s Docstring: Derive dispersion relation from rectified arc lamp frame 393s 393s This recipe is used to wavelength calibrate MOS/MXU slit spectra 393s contained in the rectified arc lamp exposure produced with recipe 393s fors_extract_slits. A pattern-matching algorithm is applied as in 393s recipe fors_detect_spectra. The input spatial map is used in the 393s production of the wavelength map. Use recipe fors_wave_calib_lss for 393s LSS data, or for MOS/MXU data where all slits have the same offset. 393s For more details on this data reduction strategy please refer to the 393s FORS Pipeline User's Manual. Note that specifying an input 393s GRISM_TABLE will set some of the recipe configuration parameters to 393s default values valid for a particular grism. In the table below the 393s MXU acronym can be alternatively read as MOS. Input files: DO 393s category: Type: Explanation: Required: 393s SPATIAL_MAP_MXU Calib Spatial map Y 393s RECTIFIED_LAMP_MXU Calib Rectified arc exposure Y 393s SLIT_LOCATION_MXU Calib Slit location table Y 393s CURV_COEFF_MXU Calib Spectral curvature Y 393s MASTER_LINECAT Calib Line catalog Y 393s GRISM_TABLE Calib Grism table . 393s Output files: DO category: Data type: Explanation: 393s REDUCED_LAMP_MXU FITS image Calibrated arc lamp exposure 393s DISP_COEFF_MXU FITS table Inverse dispersion coefficients 393s DISP_RESIDUALS_MXU FITS image Image of modeling residuals 393s WAVELENGTH_MAP_MXU FITS image Wavelengths mapped on CCD 393s SPECTRAL_RESOLUTION_MXU FITS table Spectral resolution table 393s 393s Parameters: 393s dispersion: Expected spectral dispersion (Angstrom/pixel) 393s (float; default: 0.0) 393s peakdetection: Initial peak detection threshold (ADU) (float; 393s default: 0.0) 393s wdegree: Degree of wavelength calibration polynomial (int; 393s default: 0) 393s wradius: Search radius if iterating pattern-matching with 393s first-guess method (int; default: 4) 393s wreject: Rejection threshold in dispersion relation fit 393s (pixel) (float; default: 0.7) 393s wcolumn: Name of line catalog table column with wavelengths 393s (str; default: 'WLEN') 393s startwavelength: Start wavelength in spectral extraction (float; 393s default: 0.0) 393s endwavelength: End wavelength in spectral extraction (float; 393s default: 0.0) 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_pmos_calib: 393s version 5.5.7 393s Parameters: {'dispersion': 0.0, 'peakdetection': 0.0, 'wdegree': 0, 'wradius': 4, 'wreject': 0.7, 'wcolumn': 'WLEN', 'cdegree': 0, 'cmode': 1, 'startwavelength': 0.0, 'endwavelength': 0.0, 'stack_method': 'average', 'minrejection': 1, 'maxrejection': 1, 'klow': 3.0, 'khigh': 3.0, 'kiter': 999, 'ddegree': -1, 'dradius': 10, 'qc': True, 'check': False} 393s Docstring: Determination of the extraction mask 393s 393s This recipe is used to identify reference lines on PMOS arc lamp 393s exposures, and trace the spectral edges on the corresponding flat 393s field exposures. This information is used to determine the spectral 393s extraction mask to be applied in the scientific data reduction, 393s performed with the recipe fors_science. This recipe accepts both FORS1 393s and FORS2 frames. The input arc lamps and flat field exposures are 393s assumed to be obtained quasi-simultaneously, so that they would be 393s described by exactly the same instrument distortions. A line catalog 393s must be specified, containing the wavelengths of the reference arc 393s lamp lines used for the wavelength calibration. A grism table 393s (typically depending on the instrument mode, and in particular on the 393s grism used) may also be specified: this table contains a default 393s recipe parameter setting to control the way spectra are extracted for 393s a specific instrument mode, as it is used for automatic run of the 393s pipeline on Paranal and in Garching. If this table is specified, it 393s will modify the default recipe parameter setting, with the exception 393s of those parameters which have been explicitly modifyed on the command 393s line. If a grism table is not specified, the input recipe parameters 393s values will always be read from the command line, or from an esorex 393s configuration file if present, or from their generic default values 393s (that are rarely meaningful). Finally a master bias frame must be 393s input to this recipe. The products SPECTRA_DETECTION_PMOS, 393s SLIT_MAP_PMOS, and DISP_RESIDUALS_PMOS, are just created if the 393s --check parameter is set to true. The MASTER_DISTORTION_TABLE is 393s marked as required, but it is not so if all slits have different 393s offsets, and in the case of FORS1 observations made with the old 393s TK2048EB4-1 1604 chip read in windowed mode (2048x400) Input files: 393s DO category: Type: Explanation: Required: 393s SCREEN_FLAT_PMOS Raw Flat field exposures Y 393s LAMP_PMOS Raw Arc lamp exposure Y 393s MASTER_BIAS or BIAS Calib Bias frame Y 393s MASTER_LINECAT Calib Line catalog Y 393s GRISM_TABLE Calib Grism table . 393s MASTER_DISTORTION_TABLE Calib Master distortions table Y 393s Output files: DO category: Data type: Explanation: 393s MASTER_SCREEN_FLAT_PMOS FITS image Combined (sum) flat field 393s MASTER_NORM_FLAT_PMOS FITS image Normalised flat field 393s MAPPED_SCREEN_FLAT_PMOS FITS image Wavelength calibrated flat field 393s MAPPED_NORM_FLAT_PMOS FITS image Wavelength calibrated normalised 393s flat REDUCED_LAMP_PMOS FITS image Wavelength calibrated arc 393s spectrum DISP_COEFF_PMOS FITS table Inverse dispersion 393s coefficients DISP_RESIDUALS_PMOS FITS image Residuals in 393s wavelength calibration DISP_RESIDUALS_TABLE_PMOS FITS table 393s Residuals in wavelength calibration DELTA_IMAGE_PMOS FITS 393s image Offset vs linear wavelength calib WAVELENGTH_MAP_PMOS 393s FITS image Wavelength for each pixel on CCD SPECTRA_DETECTION_PMOS 393s FITS image Check for preliminary detection SLIT_MAP_PMOS 393s FITS image Map of central wavelength on CCD CURV_TRACES_PMOS 393s FITS table Spectral curvature traces CURV_COEFF_PMOS FITS 393s table Spectral curvature coefficients SPATIAL_MAP_PMOS 393s FITS image Spatial position along slit on CCD 393s SPECTRAL_RESOLUTION_PMOS FITS table Resolution at reference arc 393s lines SLIT_LOCATION_PMOS FITS table Slits on product frames 393s and CCD 393s 393s Parameters: 393s dispersion: Expected spectral dispersion (Angstrom/pixel) 393s (float; default: 0.0) 393s peakdetection: Initial peak detection threshold (ADU) (float; 393s default: 0.0) 393s wdegree: Degree of wavelength calibration polynomial (int; 393s default: 0) 393s wradius: Search radius if iterating pattern-matching with 393s first-guess method (int; default: 4) 393s wreject: Rejection threshold in dispersion relation fit 393s (pixel) (float; default: 0.7) 393s wcolumn: Name of line catalog table column with wavelengths 393s (str; default: 'WLEN') 393s cdegree: Degree of spectral curvature polynomial (int; 393s default: 0) 393s cmode: Interpolation mode of curvature solution (0 = no 393s interpolation, 1 = fill gaps, 2 = global model) 393s (int; default: 1) 393s startwavelength: Start wavelength in spectral extraction (float; 393s default: 0.0) 393s endwavelength: End wavelength in spectral extraction (float; 393s default: 0.0) 393s stack_method: Frames combination method (str; default: 'average') 393s minrejection: Number of lowest values to be rejected (int; 393s default: 1) 393s maxrejection: Number of highest values to be rejected (int; 393s default: 1) 393s klow: Low threshold in ksigma method (float; default: 3.0) 393s khigh: High threshold in ksigma method (float; default: 393s 3.0) 393s kiter: Max number of iterations in ksigma method (int; 393s default: 999) 393s ddegree: Degree of flat field fitting polynomial along 393s dispersion direction (int; default: -1) 393s dradius: Smooth box radius for flat field along dispersion 393s direction (int; default: 10) 393s qc: Compute QC1 parameters (bool; default: True) 393s check: Create intermediate products (bool; default: False) 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_extract_objects: 393s version 5.5.7 393s Parameters: {'ext_mode': 1} 393s Docstring: Extract objects in slit spectra 393s 393s This recipe is used to extract scientific objects spectra on a 393s resampled image produced with recipe fors_resample, at the positions 393s listed in the object table produced by recipe fors_detect_objects. 393s Please refer to the FORS Pipeline User's Manual for more details on 393s object extraction. In the table below the MXU acronym can be 393s alternatively read as MOS and LSS, and SCI as STD. Input files: DO 393s category: Type: Explanation: Required: 393s MAPPED_SCI_MXU Calib Resampled slit spectra Y 393s MAPPED_SKY_SCI_MXU Calib Resampled sky spectra Y 393s OBJECT_TABLE_SCI_MXU Calib Object table Y 393s Output files: DO category: Data type: Explanation: 393s REDUCED_SCI_MXU FITS image Extracted object spectra 393s REDUCED_SKY_SCI_MXU FITS image Extracted sky spectra 393s REDUCED_ERROR_SCI_MXU FITS image Error on extracted spectra 393s 393s Parameters: 393s ext_mode: Object extraction method: 0 = aperture, 1 = Horne optimal 393s extraction (int; default: 1) 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_pmos_extract: 393s version 5.5.7 393s Parameters: {'dispersion': 0.0, 'skyalign': 0, 'wcolumn': 'WLEN', 'startwavelength': 0.0, 'endwavelength': 0.0, 'flux': True, 'flatfield': False, 'skyglobal': False, 'skymedian': False, 'skylocal': True, 'cosmics': False, 'slit_margin': 3, 'ext_radius': 6, 'cont_radius': 0, 'ext_mode': 1, 'time_normalise': True, 'chromatism': True, 'check': False} 393s Docstring: Extraction of scientific spectra 393s 393s This recipe is used to reduce scientific spectra using the extraction 393s mask and the products created by the recipe fors_mpol_calib. The 393s spectra are bias subtracted, flat fielded (if a normalised flat field 393s is specified) and remapped eliminating the optical distortions. The 393s wavelength calibration can be optionally upgraded using a number of 393s sky lines: if no sky lines catalog of wavelengths is specified, an 393s internal one is used instead. If the alignment to the sky lines is 393s performed, the input dispersion coefficients table is upgraded and 393s saved to disk, and a new CCD wavelengths map is created. This recipe 393s accepts both FORS1 and FORS2 frames. A grism table (typically 393s depending on the instrument mode, and in particular on the grism used) 393s may also be specified: this table contains a default recipe parameter 393s setting to control the way spectra are extracted for a specific 393s instrument mode, as it is used for automatic run of the pipeline on 393s Paranal and in Garching. If this table is specified, it will modify 393s the default recipe parameter setting, with the exception of those 393s parameters which have been explicitly modifyed on the command line. If 393s a grism table is not specified, the input recipe parameters values 393s will always be read from the command line, or from an esorex 393s configuration file if present, or from their generic default values 393s (that are rarely meaningful). Either a scientific or a standard star 393s exposure can be specified in input. The acronym SCI on products should 393s be read STD in case of standard stars observations. Input files: 393s DO category: Type: Explanation: Required: 393s SCIENCE_PMOS Raw Scientific exposure Y 393s or STANDARD_PMOS Raw Standard star exposure Y 393s MASTER_BIAS Calib Master bias Y 393s GRISM_TABLE Calib Grism table . 393s MASTER_SKYLINECAT Calib Sky lines catalog . 393s MASTER_NORM_FLAT_PMOS Calib Normalised flat field . 393s DISP_COEFF_PMOS Calib Inverse dispersion Y 393s CURV_COEFF_PMOS Calib Spectral curvature Y 393s SLIT_LOCATION_PMOS Calib Slits positions table Y 393s RETARDER_WAVEPLATE_CHROMATISM Calib Chromatism correction . 393s Output files: DO category: Data type: Explanation: 393s REDUCED_SCI_PMOS FITS image Extracted scientific spectra 393s REDUCED_SKY_SCI_PMOS FITS image Extracted sky spectra 393s REDUCED_ERROR_SCI_PMOS FITS image Errors on extracted spectra 393s REDUCED_SCI_X_PMOS FITS image X Stokes parameter (and L) 393s REDUCED_ERROR_X_PMOS FITS image Error on X Stokes parameter 393s REDUCED_NUL_X_PMOS FITS image Null parameter for X 393s REDUCED_POL_ANGLE_PMOS FITS image Direction of linear 393s polarization REDUCED_POL_ANGLE_ERROR_PMOS FITS image Error on 393s polarization direction UNMAPPED_SCI_PMOS FITS image Sky 393s subtracted scientific spectra MAPPED_SCI_PMOS FITS 393s image Rectified scientific spectra MAPPED_ALL_SCI_PMOS 393s FITS image Rectified science spectra with sky MAPPED_SKY_SCI_PMOS 393s FITS image Rectified sky spectra UNMAPPED_SKY_SCI_PMOS FITS 393s image Sky on CCD GLOBAL_SKY_SPECTRUM_PMOS FITS table Global 393s sky spectrum OBJECT_TABLE_SCI_PMOS FITS table Positions of 393s detected objects OBJECT_TABLE_POL_SCI_PMOS FITS table Positions 393s of real objects Only if the sky-alignment of the wavelength 393s solution is requested: DISP_COEFF_SCI_PMOS FITS table 393s Upgraded dispersion coefficients WAVELENGTH_MAP_SCI_PMOS FITS 393s image Upgraded wavelength map 393s 393s Parameters: 393s dispersion: Resampling step (Angstrom/pixel) (float; default: 393s 0.0) 393s skyalign: Polynomial order for sky lines alignment, or -1 to 393s avoid alignment (int; default: 0) 393s wcolumn: Name of sky line catalog table column with 393s wavelengths (str; default: 'WLEN') 393s startwavelength: Start wavelength in spectral extraction (float; 393s default: 0.0) 393s endwavelength: End wavelength in spectral extraction (float; 393s default: 0.0) 393s flux: Apply flux conservation (bool; default: True) 393s flatfield: Apply flat field (bool; default: False) 393s skyglobal: Subtract global sky spectrum from CCD (bool; 393s default: False) 393s skymedian: Sky subtraction from extracted slit spectra (bool; 393s default: False) 393s skylocal: Sky subtraction from CCD slit spectra (bool; 393s default: True) 393s cosmics: Eliminate cosmic rays hits (only if global sky 393s subtraction is also requested) (bool; default: 393s False) 393s slit_margin: Number of pixels to exclude at each slit in object 393s detection and extraction (int; default: 3) 393s ext_radius: Maximum extraction radius for detected objects 393s (pixel) (int; default: 6) 393s cont_radius: Minimum distance at which two objects of equal 393s luminosity do not contaminate each other (pixel) 393s (int; default: 0) 393s ext_mode: Object extraction method: 0 = aperture, 1 = Horne 393s optimal extraction (int; default: 1) 393s time_normalise: Normalise output spectra by the exposure time (bool; 393s default: True) 393s chromatism: Chromatism correction to polarization angles (bool; 393s default: True) 393s check: Create intermediate products (bool; default: False) 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_align_sky: 393s version 5.5.7 393s Parameters: {'dispersion': 0.0, 'startwavelength': 0.0, 'endwavelength': 0.0, 'skyalign': 0, 'wcolumn': 'WLEN'} 393s Docstring: Upgrade wavelength solution using sky lines 393s 393s This recipe is used to align the wavelength solution based on the arc 393s lamp exposure on a set of sky lines observed on a scientific exposure. 393s The input rectified frames are produced by the recipe 393s fors_extract_slits. An input catalog of sky lines can be specified, 393s otherwise an internal one is used. This recipe should be applied to 393s multi-slit MOS/MXU data: for LSS or long-slit like data (MOS/MXU with 393s all slits at the same offset) use recipe fors_align_sky_lss instead. 393s Please refer to the FORS Pipeline User's Manual for more details. In 393s the table below the MXU acronym can be alternatively read as MOS, and 393s SCI as STD. Input files: DO category: Type: 393s Explanation: Required: RECTIFIED_ALL_SCI_MXU or 393s RECTIFIED_SKY_SCI_MXU Calib Frame with sky lines Y 393s SPATIAL_MAP_MXU Calib Spatial coordinate map Y 393s CURV_COEFF_MXU Calib Spectral curvature Y 393s SLIT_LOCATION_MXU Calib Slit location on CCD Y 393s DISP_COEFF_MXU Calib Dispersion solution Y 393s MASTER_SKYLINECAT Calib Catalog of sky lines . 393s GRISM_TABLE Calib Grism table . 393s Output files: DO category: Data type: Explanation: 393s SKY_SHIFTS_SLIT_SCI_MXU FITS table Observed sky lines offsets 393s WAVELENGTH_MAP_SCI_MXU FITS image Wavelength mapped on CCD 393s DISP_COEFF_SCI_MXU FITS image Upgraded dispersion solution 393s 393s Parameters: 393s dispersion: Expected spectral dispersion (Angstrom/pixel) 393s (float; default: 0.0) 393s startwavelength: Start wavelength in spectral extraction (float; 393s default: 0.0) 393s endwavelength: End wavelength in spectral extraction (float; 393s default: 0.0) 393s skyalign: Polynomial order for sky lines alignment (int; 393s default: 0) 393s wcolumn: Name of sky line catalog table column with 393s wavelengths (str; default: 'WLEN') 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_sumflux: 393s version 5.5.7 393s Parameters: {'xlow': 0, 'ylow': 0, 'xhigh': 0, 'yhigh': 0} 393s Docstring: Integrate flux from all or part of the input frame 393s 393s This recipe is used to monitor any lamp flux on the CCD. The input raw 393s image should be either a FLUX_ARC_LSS or a FLUX_FLAT_LSS frame. After 393s the background subtraction the total signal is integrated and divided 393s by the exposure time and by the total number of CCD original pixels 393s (keeping into account a possible rebinned readout). In the case of 393s FORS2 frames the background is the median level evaluated from the 393s available overscan regions. In the case of FORS1 data, where overscan 393s regions are missing, the background is evaluated as the median level 393s of the first 200 CCD columns for flat field data, while for arc lamp 393s data a background map evaluated from the regions without spectral 393s lines is computed and subtracted. The background subtracted frame is 393s written to output in all cases, and the QC parameters QC LAMP FLUX and 393s QC LAMP FLUXERR are computed. Input files: DO category: Type: 393s Explanation: Required: FLUX_FLAT_LSS Raw Flat 393s field exposure Y or FLUX_ARC_LSS Raw Arc lamp exposure 393s Y Output files: DO category: Data type: Explanation: 393s FLUX_LAMP_LSS FITS image Background subtracted integration region 393s 393s Parameters: 393s xlow: X coordinate of lower left corner of integration region 393s (pixel) (int; default: 0) 393s ylow: Y coordinate of lower left corner of integration region 393s (pixel) (int; default: 0) 393s xhigh: X coordinate of upper right corner of integration region 393s (pixel) (0 = CCD size) (int; default: 0) 393s yhigh: Y coordinate of upper right corner of integration region 393s (pixel) (0 = CCD size) (int; default: 0) 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_dark: 393s version 5.5.7 393s Parameters: {'stack_method': 'median', 'minrejection': 1, 'maxrejection': 1, 'klow': 3.0, 'khigh': 3.0, 'kiter': 999} 393s Docstring: Compute master dark frame 393s 393s This recipe is used to combine input raw DARK frames into a master 393s dark frame by subtracing the master bias and using the given stacking 393s method. The overscan regions, if present, are removed from the result. 393s Input files: DO category: Type: Explanation: 393s Required: DARK Raw Dark frame 393s Y MASTER_BIAS FITS image Master bias Y 393s Output files: DO category: Data type: Explanation: 393s MASTER_DARK FITS image Master dark frame 393s 393s Parameters: 393s stack_method: Frames combination method (str; default: 'median') 393s minrejection: Number of lowest values to be rejected (int; default: 393s 1) 393s maxrejection: Number of highest values to be rejected (int; default: 393s 1) 393s klow: Low threshold in ksigma method (float; default: 3.0) 393s khigh: High threshold in ksigma method (float; default: 3.0) 393s kiter: Max number of iterations in ksigma method (int; 393s default: 999) 393s Author: Jonas M. Larsen 393s 393s 393s Recipe fors_img_screen_flat: 393s version 5.5.7 393s Parameters: {'stack_method': 'average', 'minrejection': 1, 'maxrejection': 1, 'klow': 3.0, 'khigh': 3.0, 'kiter': 999, 'xradius': 50, 'yradius': 50, 'degree': -1, 'sampling': 100} 393s Docstring: Compute master screen flat frame 393s 393s After bias subtraction, the input flat field frames are combined using 393s the given stack method. The combined frame is finally normalised 393s dividing it by its large scale illumination trend. The large scale 393s trend is obtained by applying a median filter with a large kernel. To 393s avoid boundary effects, the median filter is applied only to the 393s specified region. The overscan regions, if present, are removed from 393s the result. Input files: DO category: Type: 393s Explanation: Required: SCREEN_FLAT_IMG Raw 393s Screen flat field Y MASTER_BIAS Raw Master 393s bias Y Output files: DO category: Data 393s type: Explanation: MASTER_SCREEN_FLAT_IMG FITS image Master 393s screen flat field 393s 393s Parameters: 393s stack_method: Frames combination method (str; default: 'average') 393s minrejection: Number of lowest values to be rejected (int; default: 393s 1) 393s maxrejection: Number of highest values to be rejected (int; default: 393s 1) 393s klow: Low threshold in ksigma method (float; default: 3.0) 393s khigh: High threshold in ksigma method (float; default: 3.0) 393s kiter: Max number of iterations in ksigma method (int; 393s default: 999) 393s xradius: Median filter x radius (unbinned pixels) (int; default: 393s 50) 393s yradius: Median filter y radius (unbinned pixels) (int; default: 393s 50) 393s degree: Degree of fitting polynomial (int; default: -1) 393s sampling: Sampling interval for fitting (int; default: 100) 393s Author: Jonas M. Larsen 393s 393s 393s Recipe fors_resample: 393s version 5.5.7 393s Parameters: {'dispersion': 0.0, 'startwavelength': 0.0, 'endwavelength': 0.0, 'flux': True} 393s Docstring: Resample input spectra at constant wavelength step 393s 393s This recipe is used to resample at constant wavelength step spatially 393s rectified spectra. The input frames are produced using either the 393s recipe fors_extract_slits in the case of MOS/MXU multi slit exposures, 393s or the recipes fors_remove_bias and fors_flatfield in the case of LSS 393s or long-slit like MOS/MXU data. Only in case of LSS or LSS-like data 393s the SLIT_LOCATION table is required in input. Please refer to the FORS 393s Pipeline User's Manual for more details. In the table below the MXU 393s acronym can also be read as MOS and LSS, SCI can be read as STD, and 393s SCIENCE as STANDARD. Input files: DO category: Type: 393s Explanation: Required: LAMP_UNBIAS_MXU or 393s SCIENCE_UNBIAS_MXU or SCIENCE_UNFLAT_MXU or RECTIFIED_LAMP_MXU 393s or RECTIFIED_ALL_SCI_MXU or RECTIFIED_SCI_MXU or 393s RECTIFIED_SKY_SCI_MXU Calib Frame to resample Y 393s DISP_COEFF_MXU or DISP_COEFF_SCI_MXU Calib Dispersion 393s coefficients Y SLIT_LOCATION_MXU Calib Slit location 393s table Y GRISM_TABLE Calib Grism table 393s . Output files: DO category: Data type: 393s Explanation: MAPPED_LAMP_MXU or MAPPED_ALL_SCI_MXU or 393s MAPPED_SCI_MXU or MAPPED_SKY_SCI_MXU FITS image Resampled 393s spectra 393s 393s Parameters: 393s dispersion: Expected spectral dispersion (Angstrom/pixel) 393s (float; default: 0.0) 393s startwavelength: Start wavelength in spectral extraction (float; 393s default: 0.0) 393s endwavelength: End wavelength in spectral extraction (float; 393s default: 0.0) 393s flux: Apply flux conservation (bool; default: True) 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_img_sky_flat: 393s version 5.5.7 393s Parameters: {'stack_method': 'median', 'minrejection': 1, 'maxrejection': 1, 'klow': 3.0, 'khigh': 3.0, 'kiter': 999} 393s Docstring: Compute master img_sky_flat frame 393s 393s Input files: DO category: Type: Explanation: 393s Number: SKY_FLAT_IMG Raw Jittered sky flat 393s fields 1+ MASTER_BIAS FITS image Master bias 393s 1 Output files: DO category: Data type: Explanation: 393s MASTER_SKY_FLAT_IMG FITS image Master sky flat field 393s 393s Parameters: 393s stack_method: Frames combination method (str; default: 'median') 393s minrejection: Number of lowest values to be rejected (int; default: 393s 1) 393s maxrejection: Number of highest values to be rejected (int; default: 393s 1) 393s klow: Low threshold in ksigma method (float; default: 3.0) 393s khigh: High threshold in ksigma method (float; default: 3.0) 393s kiter: Max number of iterations in ksigma method (int; 393s default: 999) 393s Author: Jonas M. Larsen 393s 393s 393s Recipe fors_science: 393s version 5.5.7 393s Parameters: {'skyalign': -1, 'flatfield': True, 'skyglobal': False, 'skymedian': False, 'skylocal': True, 'cosmics': False, 'slit_margin': 3, 'ext_radius': 12, 'cont_radius': 0, 'ext_mode': 1, 'resp_fit_nknots': -2, 'resp_fit_degree': -2, 'resp_ignore_mode': 'stellar_absorption,telluric,command_line', 'resp_ignore_points': '', 'resp_use_flat_sed': 'grism_table', 'nonlinear_level': 60000.0, 'generate_idp': True} 393s Docstring: Extraction of scientific spectra 393s 393s This recipe is used to reduce scientific spectra using the extraction 393s mask and the products created by the recipe fors_calib. The spectra 393s are bias subtracted, flat fielded (if a normalised flat field is 393s specified) and remapped eliminating the optical distortions. The 393s wavelength calibration can be optionally upgraded using a number of 393s sky lines: if no sky lines catalog of wavelengths is specified, an 393s internal one is used instead. If the alignment to the sky lines is 393s performed, the input dispersion coefficients table is upgraded and 393s saved to disk, and a new CCD wavelengths map is created. This recipe 393s accepts both FORS1 and FORS2 frames. A grism table (typically 393s depending on the instrument mode, and in particular on the grism used) 393s may also be specified: this table contains a default recipe parameter 393s setting to control the way spectra are extracted for a specific 393s instrument mode, as it is used for automatic run of the pipeline on 393s Paranal and in Garching. If this table is specified, it will modify 393s the default recipe parameter setting, with the exception of those 393s parameters which have been explicitly modifyed on the command line. If 393s a grism table is not specified, the input recipe parameters values 393s will always be read from the command line, or from an esorex 393s configuration file if present, or from their generic default values 393s (that are rarely meaningful). In the table below the MXU acronym can 393s be read alternatively as MOS and LSS, depending on the instrument mode 393s of the input data. The acronym SCI on products should be read STD in 393s case of standard stars observations A CURV_COEFF table is not (yet) 393s expected for LSS data. Either a scientific or a standard star exposure 393s can be specified in input. Only in case of a standard star exposure 393s input, the atmospheric extinction table and a table with the physical 393s fluxes of the observed standard star must be specified in input, and a 393s spectro-photometric table is created in output. This table can then be 393s input again to this recipe, always with an atmospheric extinction 393s table, and if a photometric calibration is requested then flux 393s calibrated spectra (in units of erg/cm/cm/s/Angstrom) are also written 393s in output. Input files: DO category: Type: 393s Explanation: Required: SCIENCE_MXU Raw 393s Scientific exposure Y or STANDARD_MXU Raw 393s Standard star exposure Y MASTER_BIAS Calib 393s Master bias Y GRISM_TABLE Calib 393s Grism table . MASTER_SKYLINECAT Calib 393s Sky lines catalog . MASTER_NORM_FLAT_MXU Calib 393s Normalised flat field . DISP_COEFF_MXU Calib 393s Inverse dispersion Y CURV_COEFF_MXU Calib 393s Spectral curvature Y SLIT_LOCATION_MXU Calib 393s Slits positions table Y FLAT_SED_MXU Calib 393s Slits dispersion profile . or, in case of LSS-like MOS/MXU data, 393s MASTER_NORM_FLAT_LONG_MXU Calib Normalised flat field . 393s DISP_COEFF_LONG_MXU Calib Inverse dispersion Y 393s SLIT_LOCATION_LONG_MXU Calib Slits positions table Y 393s GLOBAL_DISTORTION_TABLE Calib Global distortion . 393s In case STANDARD_MXU is specified in input, EXTINCT_TABLE 393s Calib Atmospheric extinction Y STD_FLUX_TABLE 393s Calib Standard star flux Y TELLURIC_CONTAMINATION 393s Calib Telluric regions list . The following input files 393s are mandatory if photometric calibrated spectra are desired: 393s EXTINCT_TABLE Calib Atmospheric extinction Y 393s SPECPHOT_TABLE Calib Response curves Y 393s If requested for standard star data, the SPECPHOT_TABLE can be 393s dropped: in this case the correction is applied using the 393s SPECPHOT_TABLE produced in the same run. Output files: DO 393s category: Data type: Explanation: REDUCED_SCI_MXU 393s FITS image Extracted scientific spectra REDUCED_SKY_SCI_MXU 393s FITS image Extracted sky spectra REDUCED_ERROR_SCI_MXU FITS 393s image Errors on extracted spectra UNMAPPED_SCI_MXU FITS 393s image Sky subtracted scientific spectra MAPPED_SCI_MXU 393s FITS image Rectified scientific spectra MAPPED_ALL_SCI_MXU 393s FITS image Rectified science spectra with sky MAPPED_SKY_SCI_MXU 393s FITS image Rectified sky spectra UNMAPPED_SKY_SCI_MXU FITS 393s image Sky on CCD OBJECT_TABLE_SCI_MXU FITS table Positions 393s of detected objects Only if the global sky subtraction is 393s requested: GLOBAL_SKY_SPECTRUM_MXU FITS table Global sky 393s spectrum Only if the sky-alignment of the wavelength solution is 393s requested: SKY_SHIFTS_LONG_SCI_MXU FITS table Sky lines offsets 393s (LSS-like data) or SKY_SHIFTS_SLIT_SCI_MXU FITS table Sky lines 393s offsets (MOS-like data) DISP_COEFF_SCI_MXU FITS table 393s Upgraded dispersion coefficients WAVELENGTH_MAP_SCI_MXU FITS 393s image Upgraded wavelength map Only if a STANDARD_MXU is specified 393s in input: SPECPHOT_TABLE FITS table Efficiency and 393s response curves Only if a photometric calibration was requested: 393s REDUCED_FLUX_SCI_MXU FITS image Flux calibrated scientific 393s spectra REDUCED_FLUX_ERROR_SCI_MXU FITS image Errors on flux 393s calibrated spectra MAPPED_FLUX_SCI_MXU FITS image Flux 393s calibrated slit spectra 393s 393s Parameters: 393s skyalign: Polynomial order for sky lines alignment, or -1 393s to avoid alignment (int; default: -1) 393s flatfield: Apply flat field (bool; default: True) 393s skyglobal: Subtract global sky spectrum from CCD (bool; 393s default: False) 393s skymedian: Sky subtraction from extracted slit spectra 393s (bool; default: False) 393s skylocal: Sky subtraction from CCD slit spectra (bool; 393s default: True) 393s cosmics: Eliminate cosmic rays hits, only if either global 393s or local (not for LSS) sky subtraction is also 393s requested. (bool; default: False) 393s slit_margin: Number of pixels to exclude at each slit in 393s object detection and extraction (int; default: 3) 393s ext_radius: Maximum extraction radius for detected objects 393s (unbinned pixel) (int; default: 12) 393s cont_radius: Minimum distance at which two objects of equal 393s luminosity do not contaminate each other (pixel) 393s (int; default: 0) 393s ext_mode: Object extraction method: 0 = aperture, 1 = Horne 393s optimal extraction (int; default: 1) 393s resp_fit_nknots: Number of knots in spline fitting of the 393s instrument response. (-1: No fitting. -2: Read 393s from grism table) (int; default: -2) 393s resp_fit_degree: Degree of polynomial in fitting of the instrument 393s response. (-1: No fitting. -2: Read from grism 393s table) (int; default: -2) 393s resp_ignore_mode: Types of lines/regions to ignore in response. 393s Valid ones are 'stellar_absorption', 'telluric' 393s and 'command_line' (from parameter 393s resp_ignore_lines) (str; default: 393s 'stellar_absorption,telluric,command_line') 393s resp_ignore_points: Extra lines/regions to ignore in response. Use a 393s comma separated list of values. A range can be 393s specified like 4500.0-4600.0 (str; default: '') 393s resp_use_flat_sed: Use the flat SED to normalise the observed 393s spectra. Value are true, false, grism_table. 393s (str; default: 'grism_table') 393s nonlinear_level: Level above which the detector is not linear 393s (float; default: 60000.0) 393s generate_idp: Set to TRUE to request IDP generation (bool; 393s default: True) 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_subtract_sky: 393s version 5.5.7 393s Parameters: {'dispersion': 0.0, 'startwavelength': 0.0, 'endwavelength': 0.0, 'cosmics': False} 393s Docstring: Subtract sky from scientific spectra 393s 393s This recipe is used to subtract the sky emission from unrebinned slit 393s spectra. This is obtained by robust fitting (i.e., excluding the 393s signal from possible point-like objects in slit) of the emission along 393s the CCD columns within each spectrum). This method doesn't work if 393s extended objects are in slit (it really destroys the object spectra), 393s and is not applicable to LSS data. The input scientific frames are 393s produced by the recipes fors_remove_bias and fors_flatfield. This 393s recipe cannot be applied to LSS or long-slit like data (MOS/MXU with 393s all slits at the same offset). No automatic recipe is available for 393s this. Please refer to the FORS Pipeline User's Manual for more 393s details. In the table below the MXU acronym can be alternatively read 393s as MOS, and SCI as STD. Input files: DO category: 393s Type: Explanation: Required: SCIENCE_UNBIAS_MXU or 393s SCIENCE_UNFLAT_MXU or STANDARD_UNBIAS_MXU or STANDARD_UNFLAT_MXU 393s Calib Frame with sky lines Y CURV_COEFF_MXU 393s Calib Spectral curvature Y SLIT_LOCATION_MXU 393s Calib Slit location on CCD Y GRISM_TABLE 393s Calib Grism table . Output files: DO category: 393s Data type: Explanation: UNMAPPED_SCI_MXU or UNMAPPED_STD_MXU 393s FITS image Sky subtracted scientific frame UNMAPPED_SKY_SCI_MXU 393s or UNMAPPED_SKY_STD_MXU FITS image Subtracted sky frame 393s 393s Parameters: 393s dispersion: Expected spectral dispersion (Angstrom/pixel) 393s (float; default: 0.0) 393s startwavelength: Start wavelength in spectral extraction (float; 393s default: 0.0) 393s endwavelength: End wavelength in spectral extraction (float; 393s default: 0.0) 393s cosmics: Eliminate cosmic rays hits (bool; default: False) 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_detect_objects: 393s version 5.5.7 393s Parameters: {'slit_margin': 3, 'ext_radius': 6, 'cont_radius': 0} 393s Docstring: Detect objects in slit spectra 393s 393s This recipe is used to detect scientific objects spectra on a 393s resampled image produced with recipe fors_resample. Please refer to 393s the FORS Pipeline User's Manual for more details on object detection. 393s In the table below the MXU acronym can be alternatively read as MOS 393s and LSS, and SCI as STD. Input files: DO category: 393s Type: Explanation: Required: MAPPED_SCI_MXU 393s Calib Resampled slit spectra Y SLIT_LOCATION_MXU 393s Calib Slit location on image Y Output files: DO category: 393s Data type: Explanation: OBJECT_TABLE_SCI_MXU FITS table 393s Object positions in slit spectra 393s 393s Parameters: 393s slit_margin: Number of pixels to exclude at each slit in object 393s detection and extraction (int; default: 3) 393s ext_radius: Maximum extraction radius for detected objects (pixel) 393s (int; default: 6) 393s cont_radius: Minimum distance at which two objects of equal 393s luminosity do not contaminate each other (pixel) (int; 393s default: 0) 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_subtract_sky_lss: 393s version 5.5.7 393s Parameters: {} 393s Docstring: Subtract sky from calibrated long slit exposure 393s 393s This recipe is used to subtract the sky from wavelength calibrated 393s scientific spectra produced by the recipe fors_resample. A simple 393s median signal level is subtracted from each image column. In the table 393s below the MXU acronym can be read alternatively as MOS and LSS, 393s depending on the instrument mode of the input data. The acronym SCI 393s may be read STD in case of standard stars observations. Note that only 393s LSS or LSS-like MOS/MXU data are to be processed by this recipe. 393s Input files: DO category: Type: Explanation: 393s Required: MAPPED_ALL_SCI_MXU Raw Scientific exposure 393s Y Output files: DO category: Data type: 393s Explanation: MAPPED_SCI_MXU FITS image Rectified 393s scientific spectra MAPPED_SKY_SCI_MXU FITS image Rectified 393s sky spectra 393s 393s No parameters 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_zeropoint: 393s version 5.5.7 393s Parameters: {'sex_exe': '/usr/bin/source-extractor', 'sex_config': '/usr/share/cpl-plugins/fors-5.5.7/config/fors.sex', 'sex_mag': 'MAG_APER', 'sex_magerr': 'MAGERR_APER', 'sex_radius': 64, 'maxoffset': 150.0, 'magcutE': 1.0, 'magcutk': 5.0, 'magsyserr': 0.01} 393s Docstring: Compute zeropoint 393s 393s Input files: DO category: Type: Explanation: 393s Number: STANDARD_IMG FITS image Phot. standard field 393s 1 MASTER_BIAS FITS image Master bias 393s 1 MASTER_SKY_FLAT_IMG FITS image Master sky flatfield 393s 1 FLX_STD_IMG FITS table Standard star catalog 393s 1+ PHOT_TABLE FITS table Filter ext. coeff, color 393s 1 Output files: DO category: Data type: Explanation: 393s SOURCES_STD_IMG FITS image Unfiltered SExtractor output 393s ALIGNED_PHOT FITS table PHOT_BACKGROUND_STD_IMG 393s FITS image Reduced science image background STANDARD_REDUCED_IMG 393s FITS image Reduced std image 393s 393s Parameters: 393s sex_exe: SExtractor executable (str; default: '/usr/bin/source- 393s extractor') 393s sex_config: SExtractor configuration file (str; default: 393s '/usr/share/cpl- plugins/fors-5.5.7/config/fors.sex') 393s sex_mag: SExtractor magnitude (str; default: 'MAG_APER') 393s sex_magerr: SExtractor magnitude error (str; default: 'MAGERR_APER') 393s sex_radius: Background error map median filter radius (unbinned 393s pixels) (int; default: 64) 393s maxoffset: Maximum acceptable offset between the image and catalogue 393s WCS (pixels) (float; default: 150.0) 393s magcutE: Zeropoint absolute cutoff (magnitude) (float; default: 393s 1.0) 393s magcutk: Zeropoint kappa rejection parameter (float; default: 5.0) 393s magsyserr: Systematic error in magnitude (float; default: 0.01) 393s Author: Jonas M. Larsen 393s 393s 393s Recipe fors_remove_bias: 393s version 5.5.7 393s Parameters: {} 393s Docstring: Subtract bias from input frame 393s 393s This recipe is used to subtract the overscan and master bias(produced 393s by the recipe fors_bias) from one raw data frame. The overscan 393s regions, if present, are used to compensate for variations of the 393s overall bias level between master bias and input raw frame. The 393s overscan regions are then trimmed from the result. The recipe should 393s allow any fors frame. Input files: DO category: 393s Type: Explanation: Required: ANY_CAT 393s Raw Raw data frame Y MASTER_BIAS 393s Calib Master bias frame Y Output files: DO category: 393s Data type: Explanation: ANY_CAT_UNBIAS FITS image Bias 393s subtracted frame 393s 393s No parameters 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_extract: 393s version 5.5.7 393s Parameters: {'dispersion': 0.0, 'skyalign': 0, 'wcolumn': 'WLEN', 'startwavelength': 0.0, 'endwavelength': 0.0, 'flux': True, 'flatfield': False, 'skyglobal': False, 'skymedian': False, 'skylocal': True, 'cosmics': False, 'slit_margin': 3, 'ext_radius': 6, 'cont_radius': 0, 'ext_mode': 1, 'time_normalise': True} 393s Docstring: Extraction of scientific spectra 393s 393s This recipe is used to reduce scientific spectra using the global 393s distortion table created by the recipe fors_calib. The spectra are 393s bias subtracted, flat fielded (if a normalised flat field is 393s specified) and remapped eliminating the optical distortions. The 393s wavelength calibration can be optionally upgraded using a number of 393s sky lines: if no sky lines catalog of wavelengths is specified, an 393s internal one is used instead. If the alignment to the sky lines is 393s performed, the applied dispersion coefficient table is upgraded and 393s saved to disk, and a new CCD wavelengths map is created. This recipe 393s accepts both FORS1 and FORS2 frames. A grism table (typically 393s depending on the instrument mode, and in particular on the grism used) 393s may also be specified: this table contains a default recipe parameter 393s setting to control the way spectra are extracted for a specific 393s instrument mode, as it is used for automatic run of the pipeline on 393s Paranal and in Garching. If this table is specified, it will modify 393s the default recipe parameter setting, with the exception of those 393s parameters which have been explicitly modifyed on the command line. If 393s a grism table is not specified, the input recipe parameters values 393s will always be read from the command line, or from an esorex 393s configuration file if present, or from their generic default values 393s (that are rarely meaningful). In the table below the MXU acronym can 393s be read alternatively as MOS and LSS, depending on the instrument mode 393s of the input data. Either a scientific or a standard star exposure can 393s be specified in input (not both). Input files: DO category: 393s Type: Explanation: Required: SCIENCE_MXU 393s Raw Scientific exposure Y or STANDARD_MXU Raw 393s Standard star exposure Y MASTER_BIAS Calib 393s Master bias Y GRISM_TABLE Calib 393s Grism table . MASTER_SKYLINECAT Calib Sky 393s lines catalog . MASTER_NORM_FLAT_MXU Calib 393s Normalised flat field . MASTER_DISTORTION_TABLE Calib 393s Global distortion model . or, in case of LSS-like MOS/MXU data, 393s MASTER_NORM_FLAT_LONG_MXU Calib Normalised flat field . 393s Output files: DO category: Data type: Explanation: 393s REDUCED_SCI_MXU FITS image Extracted scientific spectra 393s REDUCED_SKY_SCI_MXU FITS image Extracted sky spectra 393s REDUCED_ERROR_SCI_MXU FITS image Errors on extracted spectra 393s UNMAPPED_SCI_MXU FITS image Sky subtracted scientific 393s spectra MAPPED_SCI_MXU FITS image Rectified scientific 393s spectra MAPPED_ALL_SCI_MXU FITS image Rectified science 393s spectra with sky MAPPED_SKY_SCI_MXU FITS image Rectified 393s sky spectra UNMAPPED_SKY_SCI_MXU FITS image Sky on CCD 393s GLOBAL_SKY_SPECTRUM_MXU FITS table Global sky spectrum 393s OBJECT_TABLE_SCI_MXU FITS table Positions of detected objects 393s Only if the sky-alignment of the wavelength solution is requested: 393s SKY_SHIFTS_LONG_SCI_MXU FITS table Sky lines offsets (LSS-like 393s data) or SKY_SHIFTS_SLIT_SCI_MXU FITS table Sky lines offsets (MOS- 393s like data) DISP_COEFF_SCI_MXU FITS table Upgraded 393s dispersion coefficients WAVELENGTH_MAP_SCI_MXU FITS image 393s Upgraded wavelength map 393s 393s Parameters: 393s dispersion: Resampling step (Angstrom/pixel) (float; default: 393s 0.0) 393s skyalign: Polynomial order for sky lines alignment, or -1 to 393s avoid alignment (int; default: 0) 393s wcolumn: Name of sky line catalog table column with 393s wavelengths (str; default: 'WLEN') 393s startwavelength: Start wavelength in spectral extraction (float; 393s default: 0.0) 393s endwavelength: End wavelength in spectral extraction (float; 393s default: 0.0) 393s flux: Apply flux conservation (bool; default: True) 393s flatfield: Apply flat field (bool; default: False) 393s skyglobal: Subtract global sky spectrum from CCD (bool; 393s default: False) 393s skymedian: Sky subtraction from extracted slit spectra (bool; 393s default: False) 393s skylocal: Sky subtraction from CCD slit spectra (bool; 393s default: True) 393s cosmics: Eliminate cosmic rays hits (only if global sky 393s subtraction is also requested) (bool; default: 393s False) 393s slit_margin: Number of pixels to exclude at each slit in object 393s detection and extraction (int; default: 3) 393s ext_radius: Maximum extraction radius for detected objects 393s (pixel) (int; default: 6) 393s cont_radius: Minimum distance at which two objects of equal 393s luminosity do not contaminate each other (pixel) 393s (int; default: 0) 393s ext_mode: Object extraction method: 0 = aperture, 1 = Horne 393s optimal extraction (int; default: 1) 393s time_normalise: Normalise output spectra by the exposure time (bool; 393s default: True) 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_spec_mflat: 393s version 5.5.7 393s Parameters: {'smooth_sed': 0.0, 'stack_method': 'sum', 'klow': 3.0, 'khigh': 3.0, 'kiter': 999, 'nonlinear_level': 50000.0, 'max_nonlinear_ratio': 0.2} 393s Docstring: Computes master spectroscopic flat, removing bias first 393s 393s This recipe is used to subtract the master bias, produced by the 393s recipe fors_bias, from a set of raw flat field frames. The input raw 393s frames are summed, the master bias frame is rescaled accordingly, and 393s subtracted from the result. The overscan regions, if present, are used 393s to compensate for variations of the bias level between master bias and 393s input raw frames. The overscan regions are then trimmed from the 393s result. In the table below the MXU acronym can be alternatively read 393s as MOS and LSS. Input files: DO category: Type: 393s Explanation: Required: SCREEN_FLAT_MXU Raw 393s Raw data frame Y SLIT_LOCATION_MXU Calib 393s Slits positions on CCD Y CURV_COEFF_MXU Calib 393s Slits tracing fits Y DISP_COEFF_MXU Calib 393s Wavelength calibration Y MASTER_BIAS Calib 393s Master bias frame Y Output files: DO category: 393s Data type: Explanation: MASTER_SCREEN_FLAT_MXU FITS image Bias 393s subtracted sum frame 393s 393s Parameters: 393s smooth_sed: Smoothing size for each flat sed (float; 393s default: 0.0) 393s stack_method: Frames combination method (str; default: 'sum') 393s klow: Low threshold in ksigma method (float; default: 393s 3.0) 393s khigh: High threshold in ksigma method (float; default: 393s 3.0) 393s kiter: Max number of iterations in ksigma method (int; 393s default: 999) 393s nonlinear_level: Level above which the detector is not linear 393s (float; default: 50000.0) 393s max_nonlinear_ratio: Maximum allowed ratio of non-linear pixels per 393s slit (float; default: 0.2) 393s Author: Carlo Izzo 393s 393s 393s Recipe fors_bias: 393s version 5.5.7 393s Parameters: {'stack_method': 'minmax', 'minrejection': 1, 'maxrejection': 1, 'klow': 3.0, 'khigh': 3.0, 'kiter': 999} 393s Docstring: Compute the master bias frame 393s 393s This recipe is used to combine input raw BIAS frames into a master 393s bias frame. The overscan regions, if present, are removed from the 393s result. Input files: DO category: Type: 393s Explanation: Required: BIAS Raw 393s Bias frame Y Output files: DO category: 393s Data type: Explanation: MASTER_BIAS FITS image 393s Master bias frame 393s 393s Parameters: 393s stack_method: Frames combination method (str; default: 'minmax') 393s minrejection: Number of lowest values to be rejected (int; default: 393s 1) 393s maxrejection: Number of highest values to be rejected (int; default: 393s 1) 393s klow: Low threshold in ksigma method (float; default: 3.0) 393s khigh: High threshold in ksigma method (float; default: 3.0) 393s kiter: Max number of iterations in ksigma method (int; 393s default: 999) 393s Author: Jonas M. Larsen, Carlo Izzo 393s 393s 393s autopkgtest [00:58:52]: test test-recipe.py: -----------------------] 394s autopkgtest [00:58:53]: test test-recipe.py: - - - - - - - - - - results - - - - - - - - - - 394s test-recipe.py PASS (superficial) 395s autopkgtest [00:58:54]: @@@@@@@@@@@@@@@@@@@@ summary 395s test-recipe.py PASS (superficial) 406s Creating nova instance adt-noble-arm64-cpl-plugin-fors-20240419-005219-juju-7f2275-prod-proposed-migration-environment-2-e7495478-db50-4826-bd1b-53dcb506d97d from image adt/ubuntu-noble-arm64-server-20240418.img (UUID 6f8e97a7-9a55-4e99-9797-31213b709dd4)...