0s autopkgtest [00:32:50]: starting date and time: 2024-04-19 00:32:50+0000 0s autopkgtest [00:32:50]: git checkout: 43bc6cdf gitlab-ci: do not include the salsa pipeline 0s autopkgtest [00:32:50]: host juju-7f2275-prod-proposed-migration-environment-3; command line: /home/ubuntu/autopkgtest/runner/autopkgtest --output-dir /tmp/autopkgtest-work.kaazrc54/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-3@bos01-s390x-22.secgroup --name adt-noble-s390x-cpl-plugin-fors-20240419-003250-juju-7f2275-prod-proposed-migration-environment-3-8a555430-b58f-4cdc-b33c-6bd5ce2c593d --image adt/ubuntu-noble-s390x-server --keyname testbed-juju-7f2275-prod-proposed-migration-environment-3 --net-id=net_prod-proposed-migration -e TERM=linux -e ''"'"'http_proxy=http://squid.internal:3128'"'"'' -e ''"'"'https_proxy=http://squid.internal:3128'"'"'' -e ''"'"'no_proxy=127.0.0.1,127.0.1.1,login.ubuntu.com,localhost,localdomain,novalocal,internal,archive.ubuntu.com,ports.ubuntu.com,security.ubuntu.com,ddebs.ubuntu.com,changelogs.ubuntu.com,launchpadlibrarian.net,launchpadcontent.net,launchpad.net,10.24.0.0/24,keystone.ps5.canonical.com,objectstorage.prodstack5.canonical.com'"'"'' --mirror=http://us.ports.ubuntu.com/ubuntu-ports/ 149s autopkgtest [00:35:19]: testbed dpkg architecture: s390x 149s autopkgtest [00:35:19]: testbed apt version: 2.7.14build2 149s autopkgtest [00:35:19]: @@@@@@@@@@@@@@@@@@@@ test bed setup 150s Get:1 http://ftpmaster.internal/ubuntu noble-proposed InRelease [117 kB] 150s Get:2 http://ftpmaster.internal/ubuntu noble-proposed/universe Sources [376 kB] 150s Get:3 http://ftpmaster.internal/ubuntu noble-proposed/multiverse Sources [2340 B] 150s Get:4 http://ftpmaster.internal/ubuntu noble-proposed/main Sources [54.2 kB] 150s Get:5 http://ftpmaster.internal/ubuntu noble-proposed/restricted Sources [12.2 kB] 150s Get:6 http://ftpmaster.internal/ubuntu noble-proposed/main s390x Packages [95.6 kB] 150s Get:7 http://ftpmaster.internal/ubuntu noble-proposed/main s390x c-n-f Metadata [3032 B] 150s Get:8 http://ftpmaster.internal/ubuntu noble-proposed/restricted s390x Packages [976 B] 150s Get:9 http://ftpmaster.internal/ubuntu noble-proposed/restricted s390x c-n-f Metadata [116 B] 150s Get:10 http://ftpmaster.internal/ubuntu noble-proposed/universe s390x Packages [497 kB] 151s Get:11 http://ftpmaster.internal/ubuntu noble-proposed/universe s390x c-n-f Metadata [7292 B] 151s Get:12 http://ftpmaster.internal/ubuntu noble-proposed/multiverse s390x c-n-f Metadata [116 B] 152s Fetched 1166 kB in 1s (1247 kB/s) 152s Reading package lists... 153s sh: 4: dhclient: not found 154s Reading package lists... 154s Building dependency tree... 154s Reading state information... 155s Calculating upgrade... 155s The following packages will be upgraded: 155s apport apport-core-dump-handler libkeyutils1 libnuma1 make man-db 155s netcat-openbsd numactl python3-apport python3-problem-report 155s 10 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 155s Need to get 1783 kB of archives. 155s After this operation, 3072 B disk space will be freed. 155s Get:1 http://ftpmaster.internal/ubuntu noble/main s390x python3-problem-report all 2.28.1-0ubuntu1 [23.8 kB] 155s Get:2 http://ftpmaster.internal/ubuntu noble/main s390x python3-apport all 2.28.1-0ubuntu1 [92.1 kB] 155s Get:3 http://ftpmaster.internal/ubuntu noble/main s390x apport-core-dump-handler all 2.28.1-0ubuntu1 [16.8 kB] 155s Get:4 http://ftpmaster.internal/ubuntu noble/main s390x apport all 2.28.1-0ubuntu1 [83.5 kB] 155s Get:5 http://ftpmaster.internal/ubuntu noble/main s390x libkeyutils1 s390x 1.6.3-3build1 [9556 B] 155s Get:6 http://ftpmaster.internal/ubuntu noble/main s390x netcat-openbsd s390x 1.226-1ubuntu2 [44.0 kB] 155s Get:7 http://ftpmaster.internal/ubuntu noble/main s390x libnuma1 s390x 2.0.18-1build1 [25.1 kB] 155s Get:8 http://ftpmaster.internal/ubuntu noble/main s390x man-db s390x 2.12.0-4build2 [1253 kB] 156s Get:9 http://ftpmaster.internal/ubuntu noble/main s390x make s390x 4.3-4.1build2 [196 kB] 156s Get:10 http://ftpmaster.internal/ubuntu noble/main s390x numactl s390x 2.0.18-1build1 [40.0 kB] 156s Preconfiguring packages ... 156s Fetched 1783 kB in 1s (2474 kB/s) 156s (Reading database ... (Reading database ... 5% (Reading database ... 10% (Reading database ... 15% (Reading database ... 20% (Reading database ... 25% (Reading database ... 30% (Reading database ... 35% (Reading database ... 40% (Reading database ... 45% (Reading database ... 50% (Reading database ... 55% (Reading database ... 60% (Reading database ... 65% (Reading database ... 70% (Reading database ... 75% (Reading database ... 80% (Reading database ... 85% (Reading database ... 90% (Reading database ... 95% (Reading database ... 100% (Reading database ... 78323 files and directories currently installed.) 156s Preparing to unpack .../0-python3-problem-report_2.28.1-0ubuntu1_all.deb ... 156s Unpacking python3-problem-report (2.28.1-0ubuntu1) over (2.28.0-0ubuntu1) ... 156s Preparing to unpack .../1-python3-apport_2.28.1-0ubuntu1_all.deb ... 156s Unpacking python3-apport (2.28.1-0ubuntu1) over (2.28.0-0ubuntu1) ... 156s Preparing to unpack .../2-apport-core-dump-handler_2.28.1-0ubuntu1_all.deb ... 156s Unpacking apport-core-dump-handler (2.28.1-0ubuntu1) over (2.28.0-0ubuntu1) ... 156s Preparing to unpack .../3-apport_2.28.1-0ubuntu1_all.deb ... 156s Unpacking apport (2.28.1-0ubuntu1) over (2.28.0-0ubuntu1) ... 156s Preparing to unpack .../4-libkeyutils1_1.6.3-3build1_s390x.deb ... 156s Unpacking libkeyutils1:s390x (1.6.3-3build1) over (1.6.3-3) ... 156s Preparing to unpack .../5-netcat-openbsd_1.226-1ubuntu2_s390x.deb ... 156s Unpacking netcat-openbsd (1.226-1ubuntu2) over (1.226-1ubuntu1) ... 156s Preparing to unpack .../6-libnuma1_2.0.18-1build1_s390x.deb ... 156s Unpacking libnuma1:s390x (2.0.18-1build1) over (2.0.18-1) ... 156s Preparing to unpack .../7-man-db_2.12.0-4build2_s390x.deb ... 156s Unpacking man-db (2.12.0-4build2) over (2.12.0-4build1) ... 157s Preparing to unpack .../8-make_4.3-4.1build2_s390x.deb ... 157s Unpacking make (4.3-4.1build2) over (4.3-4.1build1) ... 157s Preparing to unpack .../9-numactl_2.0.18-1build1_s390x.deb ... 157s Unpacking numactl (2.0.18-1build1) over (2.0.18-1) ... 157s Setting up libkeyutils1:s390x (1.6.3-3build1) ... 157s Setting up python3-problem-report (2.28.1-0ubuntu1) ... 157s Setting up netcat-openbsd (1.226-1ubuntu2) ... 157s Setting up man-db (2.12.0-4build2) ... 157s Updating database of manual pages ... 159s man-db.service is a disabled or a static unit not running, not starting it. 159s Setting up python3-apport (2.28.1-0ubuntu1) ... 159s Setting up make (4.3-4.1build2) ... 159s Setting up libnuma1:s390x (2.0.18-1build1) ... 159s Setting up numactl (2.0.18-1build1) ... 159s Setting up apport-core-dump-handler (2.28.1-0ubuntu1) ... 161s Setting up apport (2.28.1-0ubuntu1) ... 161s Installing new version of config file /etc/apport/crashdb.conf ... 161s apport-autoreport.service is a disabled or a static unit not running, not starting it. 161s Processing triggers for libc-bin (2.39-0ubuntu8) ... 162s Reading package lists... 162s Building dependency tree... 162s Reading state information... 162s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 163s Hit:1 http://ftpmaster.internal/ubuntu noble InRelease 163s Hit:2 http://ftpmaster.internal/ubuntu noble-updates InRelease 163s Hit:3 http://ftpmaster.internal/ubuntu noble-security InRelease 163s Hit:4 http://ftpmaster.internal/ubuntu noble-proposed InRelease 164s Reading package lists... 164s Reading package lists... 164s Building dependency tree... 164s Reading state information... 164s Calculating upgrade... 164s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 165s Reading package lists... 165s Building dependency tree... 165s Reading state information... 165s 0 upgraded, 0 newly installed, 0 to remove and 0 not upgraded. 165s autopkgtest [00:35:35]: rebooting testbed after setup commands that affected boot 206s autopkgtest [00:36:16]: testbed running kernel: Linux 6.8.0-22-generic #22-Ubuntu SMP Thu Apr 4 21:54:17 UTC 2024 209s autopkgtest [00:36:19]: @@@@@@@@@@@@@@@@@@@@ apt-source cpl-plugin-fors 213s Get:1 http://ftpmaster.internal/ubuntu noble/universe cpl-plugin-fors 5.5.7+dfsg-2build1 (dsc) [2571 B] 213s Get:2 http://ftpmaster.internal/ubuntu noble/universe cpl-plugin-fors 5.5.7+dfsg-2build1 (tar) [1299 kB] 213s Get:3 http://ftpmaster.internal/ubuntu noble/universe cpl-plugin-fors 5.5.7+dfsg-2build1 (diff) [13.3 kB] 213s gpgv: Signature made Tue Dec 7 17:25:56 2021 UTC 213s gpgv: using RSA key AC483F68DE728F43F2202FCA568D30F321B2133D 213s gpgv: issuer "steve.langasek@ubuntu.com" 213s gpgv: Can't check signature: No public key 213s dpkg-source: warning: cannot verify inline signature for ./cpl-plugin-fors_5.5.7+dfsg-2build1.dsc: no acceptable signature found 213s autopkgtest [00:36:23]: testing package cpl-plugin-fors version 5.5.7+dfsg-2build1 213s autopkgtest [00:36:23]: build not needed 216s autopkgtest [00:36:26]: test test-recipe.py: preparing testbed 217s Reading package lists... 217s Building dependency tree... 217s Reading state information... 218s Starting pkgProblemResolver with broken count: 0 218s Starting 2 pkgProblemResolver with broken count: 0 218s Done 218s The following additional packages will be installed: 218s cpl-plugin-fors libblas3 libcext0 libcfitsio10t64 libcplcore26 libcpldfs26 218s libcpldrs26 libcplui26 liberfa1 libfftw3-double3 libfftw3-single3 218s libgfortran5 libgomp1 libgsl27 libgslcblas0 libjs-jquery 218s libjs-jquery-hotkeys libjs-jquery-isonscreen libjs-jquery-metadata 218s libjs-jquery-tablesorter libjs-jquery-throttle-debounce libjs-sphinxdoc 218s libjs-underscore liblapack3 libwcs8 python3-astropy 218s python3-astropy-iers-data python3-coverage python3-cpl python3-dateutil 218s python3-erfa python3-hypothesis python3-iniconfig python3-numpy 218s python3-packaging python3-pluggy python3-ply python3-pytest 218s python3-pytest-arraydiff python3-pytest-astropy 218s python3-pytest-astropy-header python3-pytest-cov python3-pytest-doctestplus 218s python3-pytest-filter-subpackage python3-pytest-mock 218s python3-pytest-remotedata python3-sortedcontainers 218s Suggested packages: 218s cpl-plugin-fors-calib cpl-plugin-fors-doc libfftw3-bin libfftw3-dev 218s gsl-ref-psdoc | gsl-doc-pdf | gsl-doc-info | gsl-ref-html libxml2-utils 218s python-astropy-doc python3-astropy-affiliated python3-bs4 python3-h5py 218s python3-matplotlib python3-pandas python-coverage-doc gdb 218s python-hypothesis-doc gcc gfortran python3-dev python-ply-doc 218s python-pytest-mock-doc python-sortedcontainers-doc 218s Recommended packages: 218s source-extractor javascript-common libjs-jquery-datatables python3-scipy 218s python3-click 218s The following NEW packages will be installed: 218s autopkgtest-satdep cpl-plugin-fors libblas3 libcext0 libcfitsio10t64 218s libcplcore26 libcpldfs26 libcpldrs26 libcplui26 liberfa1 libfftw3-double3 218s libfftw3-single3 libgfortran5 libgomp1 libgsl27 libgslcblas0 libjs-jquery 218s libjs-jquery-hotkeys libjs-jquery-isonscreen libjs-jquery-metadata 218s libjs-jquery-tablesorter libjs-jquery-throttle-debounce libjs-sphinxdoc 218s libjs-underscore liblapack3 libwcs8 python3-astropy 218s python3-astropy-iers-data python3-coverage python3-cpl python3-dateutil 218s python3-erfa python3-hypothesis python3-iniconfig python3-numpy 218s python3-packaging python3-pluggy python3-ply python3-pytest 218s python3-pytest-arraydiff python3-pytest-astropy 218s python3-pytest-astropy-header python3-pytest-cov python3-pytest-doctestplus 218s python3-pytest-filter-subpackage python3-pytest-mock 218s python3-pytest-remotedata python3-sortedcontainers 218s 0 upgraded, 48 newly installed, 0 to remove and 0 not upgraded. 218s Need to get 21.1 MB/21.1 MB of archives. 218s After this operation, 95.9 MB of additional disk space will be used. 218s Get:1 /tmp/autopkgtest.dFHrkN/1-autopkgtest-satdep.deb autopkgtest-satdep s390x 0 [728 B] 218s Get:2 http://ftpmaster.internal/ubuntu noble/main s390x libjs-jquery all 3.6.1+dfsg+~3.5.14-1 [328 kB] 219s Get:3 http://ftpmaster.internal/ubuntu noble/universe s390x libjs-jquery-hotkeys all 0~20130707+git2d51e3a9+dfsg-2ubuntu2 [11.5 kB] 219s Get:4 http://ftpmaster.internal/ubuntu noble/universe s390x libcext0 s390x 7.3.2+ds-1build3 [33.9 kB] 219s Get:5 http://ftpmaster.internal/ubuntu noble/universe s390x libcfitsio10t64 s390x 4.3.1-1.1build2 [609 kB] 219s Get:6 http://ftpmaster.internal/ubuntu noble/main s390x libgomp1 s390x 14-20240412-0ubuntu1 [151 kB] 219s Get:7 http://ftpmaster.internal/ubuntu noble/main s390x libfftw3-double3 s390x 3.3.10-1ubuntu3 [512 kB] 219s Get:8 http://ftpmaster.internal/ubuntu noble/main s390x libfftw3-single3 s390x 3.3.10-1ubuntu3 [481 kB] 219s Get:9 http://ftpmaster.internal/ubuntu noble/universe s390x libcplcore26 s390x 7.3.2+ds-1build3 [600 kB] 219s Get:10 http://ftpmaster.internal/ubuntu noble/universe s390x libcplui26 s390x 7.3.2+ds-1build3 [37.9 kB] 219s Get:11 http://ftpmaster.internal/ubuntu noble/universe s390x libcpldfs26 s390x 7.3.2+ds-1build3 [41.8 kB] 219s Get:12 http://ftpmaster.internal/ubuntu noble/universe s390x libwcs8 s390x 8.2.2+ds-3build2 [289 kB] 219s Get:13 http://ftpmaster.internal/ubuntu noble/universe s390x libcpldrs26 s390x 7.3.2+ds-1build3 [73.4 kB] 219s Get:14 http://ftpmaster.internal/ubuntu noble-proposed/universe s390x libgslcblas0 s390x 2.7.1+dfsg-6ubuntu2 [150 kB] 219s Get:15 http://ftpmaster.internal/ubuntu noble-proposed/universe s390x libgsl27 s390x 2.7.1+dfsg-6ubuntu2 [1084 kB] 219s Get:16 http://ftpmaster.internal/ubuntu noble/universe s390x cpl-plugin-fors s390x 5.5.7+dfsg-2build1 [757 kB] 219s Get:17 http://ftpmaster.internal/ubuntu noble/main s390x libblas3 s390x 3.12.0-3build1 [245 kB] 219s Get:18 http://ftpmaster.internal/ubuntu noble/main s390x libgfortran5 s390x 14-20240412-0ubuntu1 [600 kB] 219s Get:19 http://ftpmaster.internal/ubuntu noble/universe s390x libjs-jquery-metadata all 12-4 [6582 B] 219s Get:20 http://ftpmaster.internal/ubuntu noble/universe s390x libjs-jquery-tablesorter all 1:2.31.3+dfsg1-3 [193 kB] 219s Get:21 http://ftpmaster.internal/ubuntu noble/universe s390x libjs-jquery-throttle-debounce all 1.1+dfsg.1-2 [12.5 kB] 219s Get:22 http://ftpmaster.internal/ubuntu noble/main s390x libjs-underscore all 1.13.4~dfsg+~1.11.4-3 [118 kB] 219s Get:23 http://ftpmaster.internal/ubuntu noble/main s390x libjs-sphinxdoc all 7.2.6-6 [149 kB] 219s Get:24 http://ftpmaster.internal/ubuntu noble/main s390x liblapack3 s390x 3.12.0-3build1 [2976 kB] 219s Get:25 http://ftpmaster.internal/ubuntu noble/universe s390x python3-iniconfig all 1.1.1-2 [6024 B] 219s Get:26 http://ftpmaster.internal/ubuntu noble/main s390x python3-packaging all 24.0-1 [41.1 kB] 219s Get:27 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pluggy all 1.4.0-1 [20.4 kB] 219s Get:28 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pytest all 7.4.4-1 [305 kB] 219s Get:29 http://ftpmaster.internal/ubuntu noble/main s390x python3-dateutil all 2.8.2-3ubuntu1 [79.4 kB] 219s Get:30 http://ftpmaster.internal/ubuntu noble/main s390x python3-sortedcontainers all 2.4.0-2 [27.6 kB] 219s Get:31 http://ftpmaster.internal/ubuntu noble/universe s390x python3-hypothesis all 6.98.15-1 [311 kB] 219s Get:32 http://ftpmaster.internal/ubuntu noble/main s390x python3-numpy s390x 1:1.26.4+ds-6ubuntu1 [4119 kB] 220s Get:33 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pytest-arraydiff all 0.6.1-2 [10.2 kB] 220s Get:34 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pytest-astropy-header all 0.2.2-1 [8190 B] 220s Get:35 http://ftpmaster.internal/ubuntu noble/universe s390x python3-coverage s390x 7.4.4+dfsg1-0ubuntu2 [147 kB] 220s Get:36 http://ftpmaster.internal/ubuntu noble/universe s390x libjs-jquery-isonscreen all 1.2.0-1.1 [3244 B] 220s Get:37 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pytest-cov all 4.1.0-1 [21.5 kB] 220s Get:38 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pytest-doctestplus all 1.2.0-1 [23.1 kB] 220s Get:39 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pytest-filter-subpackage all 0.2.0-1 [6094 B] 220s Get:40 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pytest-mock all 3.12.0-1.1 [11.3 kB] 220s Get:41 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pytest-remotedata all 0.4.1-1 [8650 B] 220s Get:42 http://ftpmaster.internal/ubuntu noble/universe s390x python3-pytest-astropy all 0.11.0-1 [5902 B] 220s Get:43 http://ftpmaster.internal/ubuntu noble/main s390x python3-ply all 3.11-6 [46.5 kB] 220s Get:44 http://ftpmaster.internal/ubuntu noble/universe s390x python3-astropy-iers-data all 0.2024.01.01.00.33.39-1 [2046 kB] 220s Get:45 http://ftpmaster.internal/ubuntu noble/universe s390x liberfa1 s390x 2.0.1-1 [136 kB] 220s Get:46 http://ftpmaster.internal/ubuntu noble/universe s390x python3-erfa s390x 2.0.1.1+ds-3 [314 kB] 220s Get:47 http://ftpmaster.internal/ubuntu noble/universe s390x python3-astropy s390x 6.0.0-1ubuntu2 [3859 kB] 220s Get:48 http://ftpmaster.internal/ubuntu noble/universe s390x python3-cpl s390x 0.7.4-2build10 [35.1 kB] 221s Fetched 21.1 MB in 2s (9950 kB/s) 221s Selecting previously unselected package libjs-jquery. 221s (Reading database ... (Reading database ... 5% (Reading database ... 10% (Reading database ... 15% (Reading database ... 20% (Reading database ... 25% (Reading database ... 30% (Reading database ... 35% (Reading database ... 40% (Reading database ... 45% (Reading database ... 50% (Reading database ... 55% (Reading database ... 60% (Reading database ... 65% (Reading database ... 70% (Reading database ... 75% (Reading database ... 80% (Reading database ... 85% (Reading database ... 90% (Reading database ... 95% (Reading database ... 100% (Reading database ... 78322 files and directories currently installed.) 221s Preparing to unpack .../00-libjs-jquery_3.6.1+dfsg+~3.5.14-1_all.deb ... 221s Unpacking libjs-jquery (3.6.1+dfsg+~3.5.14-1) ... 221s Selecting previously unselected package libjs-jquery-hotkeys. 221s Preparing to unpack .../01-libjs-jquery-hotkeys_0~20130707+git2d51e3a9+dfsg-2ubuntu2_all.deb ... 221s Unpacking libjs-jquery-hotkeys (0~20130707+git2d51e3a9+dfsg-2ubuntu2) ... 221s Selecting previously unselected package libcext0:s390x. 221s Preparing to unpack .../02-libcext0_7.3.2+ds-1build3_s390x.deb ... 221s Unpacking libcext0:s390x (7.3.2+ds-1build3) ... 221s Selecting previously unselected package libcfitsio10t64:s390x. 221s Preparing to unpack .../03-libcfitsio10t64_4.3.1-1.1build2_s390x.deb ... 221s Unpacking libcfitsio10t64:s390x (4.3.1-1.1build2) ... 221s Selecting previously unselected package libgomp1:s390x. 221s Preparing to unpack .../04-libgomp1_14-20240412-0ubuntu1_s390x.deb ... 221s Unpacking libgomp1:s390x (14-20240412-0ubuntu1) ... 221s Selecting previously unselected package libfftw3-double3:s390x. 221s Preparing to unpack .../05-libfftw3-double3_3.3.10-1ubuntu3_s390x.deb ... 221s Unpacking libfftw3-double3:s390x (3.3.10-1ubuntu3) ... 221s Selecting previously unselected package libfftw3-single3:s390x. 221s Preparing to unpack .../06-libfftw3-single3_3.3.10-1ubuntu3_s390x.deb ... 221s Unpacking libfftw3-single3:s390x (3.3.10-1ubuntu3) ... 221s Selecting previously unselected package libcplcore26:s390x. 221s Preparing to unpack .../07-libcplcore26_7.3.2+ds-1build3_s390x.deb ... 221s Unpacking libcplcore26:s390x (7.3.2+ds-1build3) ... 221s Selecting previously unselected package libcplui26:s390x. 221s Preparing to unpack .../08-libcplui26_7.3.2+ds-1build3_s390x.deb ... 221s Unpacking libcplui26:s390x (7.3.2+ds-1build3) ... 221s Selecting previously unselected package libcpldfs26:s390x. 221s Preparing to unpack .../09-libcpldfs26_7.3.2+ds-1build3_s390x.deb ... 221s Unpacking libcpldfs26:s390x (7.3.2+ds-1build3) ... 221s Selecting previously unselected package libwcs8:s390x. 221s Preparing to unpack .../10-libwcs8_8.2.2+ds-3build2_s390x.deb ... 221s Unpacking libwcs8:s390x (8.2.2+ds-3build2) ... 221s Selecting previously unselected package libcpldrs26:s390x. 221s Preparing to unpack .../11-libcpldrs26_7.3.2+ds-1build3_s390x.deb ... 221s Unpacking libcpldrs26:s390x (7.3.2+ds-1build3) ... 221s Selecting previously unselected package libgslcblas0:s390x. 221s Preparing to unpack .../12-libgslcblas0_2.7.1+dfsg-6ubuntu2_s390x.deb ... 221s Unpacking libgslcblas0:s390x (2.7.1+dfsg-6ubuntu2) ... 221s Selecting previously unselected package libgsl27:s390x. 221s Preparing to unpack .../13-libgsl27_2.7.1+dfsg-6ubuntu2_s390x.deb ... 221s Unpacking libgsl27:s390x (2.7.1+dfsg-6ubuntu2) ... 221s Selecting previously unselected package cpl-plugin-fors:s390x. 221s Preparing to unpack .../14-cpl-plugin-fors_5.5.7+dfsg-2build1_s390x.deb ... 221s Unpacking cpl-plugin-fors:s390x (5.5.7+dfsg-2build1) ... 221s Selecting previously unselected package libblas3:s390x. 221s Preparing to unpack .../15-libblas3_3.12.0-3build1_s390x.deb ... 221s Unpacking libblas3:s390x (3.12.0-3build1) ... 221s Selecting previously unselected package libgfortran5:s390x. 221s Preparing to unpack .../16-libgfortran5_14-20240412-0ubuntu1_s390x.deb ... 221s Unpacking libgfortran5:s390x (14-20240412-0ubuntu1) ... 221s Selecting previously unselected package 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(0.7.4-2build10) ... 233s Setting up autopkgtest-satdep (0) ... 233s Processing triggers for man-db (2.12.0-4build2) ... 233s Processing triggers for libc-bin (2.39-0ubuntu8) ... 237s (Reading database ... 82245 files and directories currently installed.) 237s Removing autopkgtest-satdep (0) ... 238s autopkgtest [00:36:48]: test test-recipe.py: [----------------------- 239s Recipe fors_zeropoint: 239s version 5.5.7 239s 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} 239s Docstring: Compute zeropoint 239s 239s Input files: DO category: Type: Explanation: 239s Number: STANDARD_IMG FITS image Phot. standard field 239s 1 MASTER_BIAS FITS image Master bias 239s 1 MASTER_SKY_FLAT_IMG FITS image Master sky flatfield 239s 1 FLX_STD_IMG FITS table Standard star catalog 239s 1+ PHOT_TABLE FITS table Filter ext. coeff, color 239s 1 Output files: DO category: Data type: Explanation: 239s SOURCES_STD_IMG FITS image Unfiltered SExtractor output 239s ALIGNED_PHOT FITS table PHOT_BACKGROUND_STD_IMG 239s FITS image Reduced science image background STANDARD_REDUCED_IMG 239s FITS image Reduced std image 239s 239s Parameters: 239s sex_exe: SExtractor executable (str; default: '/usr/bin/source- 239s extractor') 239s sex_config: SExtractor configuration file (str; default: 239s '/usr/share/cpl- plugins/fors-5.5.7/config/fors.sex') 239s sex_mag: SExtractor magnitude (str; default: 'MAG_APER') 239s sex_magerr: SExtractor magnitude error (str; default: 'MAGERR_APER') 239s sex_radius: Background error map median filter radius (unbinned 239s pixels) (int; default: 64) 239s maxoffset: Maximum acceptable offset between the image and catalogue 239s WCS (pixels) (float; default: 150.0) 239s magcutE: Zeropoint absolute cutoff (magnitude) (float; default: 239s 1.0) 239s magcutk: Zeropoint kappa rejection parameter (float; default: 5.0) 239s magsyserr: Systematic error in magnitude (float; default: 0.01) 239s Author: Jonas M. Larsen 239s 239s 239s Recipe fors_detect_spectra: 239s version 5.5.7 239s 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} 239s Docstring: Detect MOS/MXU spectra on CCD 239s 239s This recipe is used to detect and locate MOS/MXU slit spectra on the 239s CCD, applying a pattern-matching algorithm. The input spectral 239s exposure must contain spectra with the dispersion direction 239s approximately horizontal, with blue on the left and red on the right. 239s Use recipe fors_wave_calib_lss for LSS data, or for MOS/MXU data where 239s all slits have the same offset. The rows of the input spectral 239s exposure are processed separately, one by one. First, the background 239s continuum is removed. Second, a list of positions of reference lines 239s candidates is created. Only peaks above a given threshold (specified 239s by the parameter --peakdetection) are selected. Third, the pattern- 239s matching task selects from the found peaks the ones corresponding to 239s the reference lines, listed in the input line catalog, associating 239s them to the appropriate wavelengths. The ensuing polynomial fit is 239s used to locate the central wavelength of the applied grism along each 239s image row. The contributions from all rows form an image of the 239s location of all spectra, that can be used as a starting point for the 239s proper modeling of the optical and spectral distortions. For more 239s details on this reduction strategy please refer to the FORS Pipeline 239s User's Manual. Note that specifying an input GRISM_TABLE will set 239s some of the recipe configuration parameters to default values valid 239s for a particular grism. Again, see the pipeline manual for more 239s details. In the table below the MXU acronym can be alternatively read 239s as MOS. Input files: DO category: Type: 239s Explanation: Required: LAMP_UNBIAS_MXU Calib 239s Bias subtracted arc Y MASTER_LINECAT Calib 239s Line catalog Y GRISM_TABLE Calib 239s Grism table . Output files: DO category: 239s Data type: Explanation: SLIT_MAP_MXU FITS image Map 239s of central wavelength on CCD SLIT_LOCATION_DETECT_MXU FITS table 239s Slits positions on CCD SPECTRA_DETECTION_MXU FITS image Check 239s of preliminary detection 239s 239s Parameters: 239s dispersion: Expected spectral dispersion (Angstrom/pixel) 239s (float; default: 0.0) 239s peakdetection: Initial peak detection threshold (ADU) (float; 239s default: 0.0) 239s wdegree: Degree of wavelength calibration polynomial (int; 239s default: 0) 239s wradius: Search radius if iterating pattern-matching with 239s first-guess method (int; default: 4) 239s wreject: Rejection threshold in dispersion relation fit 239s (pixel) (float; default: 0.7) 239s wcolumn: Name of line catalog table column with wavelengths 239s (str; default: 'WLEN') 239s startwavelength: Start wavelength in spectral extraction (float; 239s default: 0.0) 239s endwavelength: End wavelength in spectral extraction (float; 239s default: 0.0) 239s slit_ident: Attempt slit identification for MOS or MXU (bool; 239s default: True) 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_wave_calib: 239s version 5.5.7 239s Parameters: {'dispersion': 0.0, 'peakdetection': 0.0, 'wdegree': 0, 'wradius': 4, 'wreject': 0.7, 'wcolumn': 'WLEN', 'startwavelength': 0.0, 'endwavelength': 0.0} 239s Docstring: Derive dispersion relation from rectified arc lamp frame 239s 239s This recipe is used to wavelength calibrate MOS/MXU slit spectra 239s contained in the rectified arc lamp exposure produced with recipe 239s fors_extract_slits. A pattern-matching algorithm is applied as in 239s recipe fors_detect_spectra. The input spatial map is used in the 239s production of the wavelength map. Use recipe fors_wave_calib_lss for 239s LSS data, or for MOS/MXU data where all slits have the same offset. 239s For more details on this data reduction strategy please refer to the 239s FORS Pipeline User's Manual. Note that specifying an input 239s GRISM_TABLE will set some of the recipe configuration parameters to 239s default values valid for a particular grism. In the table below the 239s MXU acronym can be alternatively read as MOS. Input files: DO 239s category: Type: Explanation: Required: 239s SPATIAL_MAP_MXU Calib Spatial map Y 239s RECTIFIED_LAMP_MXU Calib Rectified arc exposure Y 239s SLIT_LOCATION_MXU Calib Slit location table Y 239s CURV_COEFF_MXU Calib Spectral curvature Y 239s MASTER_LINECAT Calib Line catalog Y 239s GRISM_TABLE Calib Grism table . 239s Output files: DO category: Data type: Explanation: 239s REDUCED_LAMP_MXU FITS image Calibrated arc lamp exposure 239s DISP_COEFF_MXU FITS table Inverse dispersion coefficients 239s DISP_RESIDUALS_MXU FITS image Image of modeling residuals 239s WAVELENGTH_MAP_MXU FITS image Wavelengths mapped on CCD 239s SPECTRAL_RESOLUTION_MXU FITS table Spectral resolution table 239s 239s Parameters: 239s dispersion: Expected spectral dispersion (Angstrom/pixel) 239s (float; default: 0.0) 239s peakdetection: Initial peak detection threshold (ADU) (float; 239s default: 0.0) 239s wdegree: Degree of wavelength calibration polynomial (int; 239s default: 0) 239s wradius: Search radius if iterating pattern-matching with 239s first-guess method (int; default: 4) 239s wreject: Rejection threshold in dispersion relation fit 239s (pixel) (float; default: 0.7) 239s wcolumn: Name of line catalog table column with wavelengths 239s (str; default: 'WLEN') 239s startwavelength: Start wavelength in spectral extraction (float; 239s default: 0.0) 239s endwavelength: End wavelength in spectral extraction (float; 239s default: 0.0) 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_science: 239s version 5.5.7 239s 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} 239s Docstring: Extraction of scientific spectra 239s 239s This recipe is used to reduce scientific spectra using the extraction 239s mask and the products created by the recipe fors_calib. The spectra 239s are bias subtracted, flat fielded (if a normalised flat field is 239s specified) and remapped eliminating the optical distortions. The 239s wavelength calibration can be optionally upgraded using a number of 239s sky lines: if no sky lines catalog of wavelengths is specified, an 239s internal one is used instead. If the alignment to the sky lines is 239s performed, the input dispersion coefficients table is upgraded and 239s saved to disk, and a new CCD wavelengths map is created. This recipe 239s accepts both FORS1 and FORS2 frames. A grism table (typically 239s depending on the instrument mode, and in particular on the grism used) 239s may also be specified: this table contains a default recipe parameter 239s setting to control the way spectra are extracted for a specific 239s instrument mode, as it is used for automatic run of the pipeline on 239s Paranal and in Garching. If this table is specified, it will modify 239s the default recipe parameter setting, with the exception of those 239s parameters which have been explicitly modifyed on the command line. If 239s a grism table is not specified, the input recipe parameters values 239s will always be read from the command line, or from an esorex 239s configuration file if present, or from their generic default values 239s (that are rarely meaningful). In the table below the MXU acronym can 239s be read alternatively as MOS and LSS, depending on the instrument mode 239s of the input data. The acronym SCI on products should be read STD in 239s case of standard stars observations A CURV_COEFF table is not (yet) 239s expected for LSS data. Either a scientific or a standard star exposure 239s can be specified in input. Only in case of a standard star exposure 239s input, the atmospheric extinction table and a table with the physical 239s fluxes of the observed standard star must be specified in input, and a 239s spectro-photometric table is created in output. This table can then be 239s input again to this recipe, always with an atmospheric extinction 239s table, and if a photometric calibration is requested then flux 239s calibrated spectra (in units of erg/cm/cm/s/Angstrom) are also written 239s in output. Input files: DO category: Type: 239s Explanation: Required: SCIENCE_MXU Raw 239s Scientific exposure Y or STANDARD_MXU Raw 239s Standard star exposure Y MASTER_BIAS Calib 239s Master bias Y GRISM_TABLE Calib 239s Grism table . MASTER_SKYLINECAT Calib 239s Sky lines catalog . MASTER_NORM_FLAT_MXU Calib 239s Normalised flat field . DISP_COEFF_MXU Calib 239s Inverse dispersion Y CURV_COEFF_MXU Calib 239s Spectral curvature Y SLIT_LOCATION_MXU Calib 239s Slits positions table Y FLAT_SED_MXU Calib 239s Slits dispersion profile . or, in case of LSS-like MOS/MXU data, 239s MASTER_NORM_FLAT_LONG_MXU Calib Normalised flat field . 239s DISP_COEFF_LONG_MXU Calib Inverse dispersion Y 239s SLIT_LOCATION_LONG_MXU Calib Slits positions table Y 239s GLOBAL_DISTORTION_TABLE Calib Global distortion . 239s In case STANDARD_MXU is specified in input, EXTINCT_TABLE 239s Calib Atmospheric extinction Y STD_FLUX_TABLE 239s Calib Standard star flux Y TELLURIC_CONTAMINATION 239s Calib Telluric regions list . The following input files 239s are mandatory if photometric calibrated spectra are desired: 239s EXTINCT_TABLE Calib Atmospheric extinction Y 239s SPECPHOT_TABLE Calib Response curves Y 239s If requested for standard star data, the SPECPHOT_TABLE can be 239s dropped: in this case the correction is applied using the 239s SPECPHOT_TABLE produced in the same run. Output files: DO 239s category: Data type: Explanation: REDUCED_SCI_MXU 239s FITS image Extracted scientific spectra REDUCED_SKY_SCI_MXU 239s FITS image Extracted sky spectra REDUCED_ERROR_SCI_MXU FITS 239s image Errors on extracted spectra UNMAPPED_SCI_MXU FITS 239s image Sky subtracted scientific spectra MAPPED_SCI_MXU 239s FITS image Rectified scientific spectra MAPPED_ALL_SCI_MXU 239s FITS image Rectified science spectra with sky MAPPED_SKY_SCI_MXU 239s FITS image Rectified sky spectra UNMAPPED_SKY_SCI_MXU FITS 239s image Sky on CCD OBJECT_TABLE_SCI_MXU FITS table Positions 239s of detected objects Only if the global sky subtraction is 239s requested: GLOBAL_SKY_SPECTRUM_MXU FITS table Global sky 239s spectrum Only if the sky-alignment of the wavelength solution is 239s requested: SKY_SHIFTS_LONG_SCI_MXU FITS table Sky lines offsets 239s (LSS-like data) or SKY_SHIFTS_SLIT_SCI_MXU FITS table Sky lines 239s offsets (MOS-like data) DISP_COEFF_SCI_MXU FITS table 239s Upgraded dispersion coefficients WAVELENGTH_MAP_SCI_MXU FITS 239s image Upgraded wavelength map Only if a STANDARD_MXU is specified 239s in input: SPECPHOT_TABLE FITS table Efficiency and 239s response curves Only if a photometric calibration was requested: 239s REDUCED_FLUX_SCI_MXU FITS image Flux calibrated scientific 239s spectra REDUCED_FLUX_ERROR_SCI_MXU FITS image Errors on flux 239s calibrated spectra MAPPED_FLUX_SCI_MXU FITS image Flux 239s calibrated slit spectra 239s 239s Parameters: 239s skyalign: Polynomial order for sky lines alignment, or -1 239s to avoid alignment (int; default: -1) 239s flatfield: Apply flat field (bool; default: True) 239s skyglobal: Subtract global sky spectrum from CCD (bool; 239s default: False) 239s skymedian: Sky subtraction from extracted slit spectra 239s (bool; default: False) 239s skylocal: Sky subtraction from CCD slit spectra (bool; 239s default: True) 239s cosmics: Eliminate cosmic rays hits, only if either global 239s or local (not for LSS) sky subtraction is also 239s requested. (bool; default: False) 239s slit_margin: Number of pixels to exclude at each slit in 239s object detection and extraction (int; default: 3) 239s ext_radius: Maximum extraction radius for detected objects 239s (unbinned pixel) (int; default: 12) 239s cont_radius: Minimum distance at which two objects of equal 239s luminosity do not contaminate each other (pixel) 239s (int; default: 0) 239s ext_mode: Object extraction method: 0 = aperture, 1 = Horne 239s optimal extraction (int; default: 1) 239s resp_fit_nknots: Number of knots in spline fitting of the 239s instrument response. (-1: No fitting. -2: Read 239s from grism table) (int; default: -2) 239s resp_fit_degree: Degree of polynomial in fitting of the instrument 239s response. (-1: No fitting. -2: Read from grism 239s table) (int; default: -2) 239s resp_ignore_mode: Types of lines/regions to ignore in response. 239s Valid ones are 'stellar_absorption', 'telluric' 239s and 'command_line' (from parameter 239s resp_ignore_lines) (str; default: 239s 'stellar_absorption,telluric,command_line') 239s resp_ignore_points: Extra lines/regions to ignore in response. Use a 239s comma separated list of values. A range can be 239s specified like 4500.0-4600.0 (str; default: '') 239s resp_use_flat_sed: Use the flat SED to normalise the observed 239s spectra. Value are true, false, grism_table. 239s (str; default: 'grism_table') 239s nonlinear_level: Level above which the detector is not linear 239s (float; default: 60000.0) 239s generate_idp: Set to TRUE to request IDP generation (bool; 239s default: True) 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_subtract_sky: 239s version 5.5.7 239s Parameters: {'dispersion': 0.0, 'startwavelength': 0.0, 'endwavelength': 0.0, 'cosmics': False} 239s Docstring: Subtract sky from scientific spectra 239s 239s This recipe is used to subtract the sky emission from unrebinned slit 239s spectra. This is obtained by robust fitting (i.e., excluding the 239s signal from possible point-like objects in slit) of the emission along 239s the CCD columns within each spectrum). This method doesn't work if 239s extended objects are in slit (it really destroys the object spectra), 239s and is not applicable to LSS data. The input scientific frames are 239s produced by the recipes fors_remove_bias and fors_flatfield. This 239s recipe cannot be applied to LSS or long-slit like data (MOS/MXU with 239s all slits at the same offset). No automatic recipe is available for 239s this. Please refer to the FORS Pipeline User's Manual for more 239s details. In the table below the MXU acronym can be alternatively read 239s as MOS, and SCI as STD. Input files: DO category: 239s Type: Explanation: Required: SCIENCE_UNBIAS_MXU or 239s SCIENCE_UNFLAT_MXU or STANDARD_UNBIAS_MXU or STANDARD_UNFLAT_MXU 239s Calib Frame with sky lines Y CURV_COEFF_MXU 239s Calib Spectral curvature Y SLIT_LOCATION_MXU 239s Calib Slit location on CCD Y GRISM_TABLE 239s Calib Grism table . Output files: DO category: 239s Data type: Explanation: UNMAPPED_SCI_MXU or UNMAPPED_STD_MXU 239s FITS image Sky subtracted scientific frame UNMAPPED_SKY_SCI_MXU 239s or UNMAPPED_SKY_STD_MXU FITS image Subtracted sky frame 239s 239s Parameters: 239s dispersion: Expected spectral dispersion (Angstrom/pixel) 239s (float; default: 0.0) 239s startwavelength: Start wavelength in spectral extraction (float; 239s default: 0.0) 239s endwavelength: End wavelength in spectral extraction (float; 239s default: 0.0) 239s cosmics: Eliminate cosmic rays hits (bool; default: False) 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_bias: 239s version 5.5.7 239s Parameters: {'stack_method': 'minmax', 'minrejection': 1, 'maxrejection': 1, 'klow': 3.0, 'khigh': 3.0, 'kiter': 999} 239s Docstring: Compute the master bias frame 239s 239s This recipe is used to combine input raw BIAS frames into a master 239s bias frame. The overscan regions, if present, are removed from the 239s result. Input files: DO category: Type: 239s Explanation: Required: BIAS Raw 239s Bias frame Y Output files: DO category: 239s Data type: Explanation: MASTER_BIAS FITS image 239s Master bias frame 239s 239s Parameters: 239s stack_method: Frames combination method (str; default: 'minmax') 239s minrejection: Number of lowest values to be rejected (int; default: 239s 1) 239s maxrejection: Number of highest values to be rejected (int; default: 239s 1) 239s klow: Low threshold in ksigma method (float; default: 3.0) 239s khigh: High threshold in ksigma method (float; default: 3.0) 239s kiter: Max number of iterations in ksigma method (int; 239s default: 999) 239s Author: Jonas M. Larsen, Carlo Izzo 239s 239s 239s Recipe fors_config: 239s version 5.5.7 239s 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'} 239s Docstring: Creation of FORS recipes configuration tables 239s 239s This recipe is used to create the so-called GRISM_TABLE, containing 239s all the FORS spectral pipeline configuration parameters related to a 239s specific grism. This is a way to provide for each specific instrument 239s mode a set of appropriate defaults for the recipe parameters. The 239s values assigned to each input parameter of fors_config are simply 239s copied to a FITS table consisting of one row, and as many columns as 239s the input parameter: each column will have the same name and type of 239s each parameter. Only the three parameters "instrument", "grism", and 239s "id" are not written to the table columns, but to the descriptor 239s header keywords INSTRUME, ESO INS GRIS1 NAME, and ESO INS GRIS1 ID, 239s that will be used by the automatic pipeline for appropriate data 239s association. Input files: none DO category: Type: 239s Explanation: Required: Output files: DO category: 239s Data type: Explanation: GRISM_TABLE FITS table 239s Recipe configuration parameters 239s 239s Parameters: 239s dispersion: Expected spectral dispersion (Angstrom/pixel) 239s (float; default: 0.0) 239s peakdetection: Peak detection threshold (ADU) (float; default: 239s 250.0) 239s wdegree: Degree of wavelength calibration polynomial (int; 239s default: 4) 239s cdegree: Degree of spectral curvature polynomial (int; 239s default: 4) 239s startwavelength: Start wavelength in spectral extraction (float; 239s default: 0.0) 239s endwavelength: End wavelength in spectral extraction (float; 239s default: 0.0) 239s instrument: Name of instrument (str; default: '0') 239s grism: Name of grism (str; default: '0') 239s grism_id: Grism ID (str; default: '0') 239s filter: Name of filter (str; default: '0') 239s filter_id: Filter ID (str; default: '0') 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_calib: 239s version 5.5.7 239s 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} 239s Docstring: Determination of the extraction mask 239s 239s This recipe is used to identify reference lines on LSS, MOS and MXU 239s arc lamp exposures, and trace the spectral edges on the corresponding 239s flat field exposures. This information is used to determine the 239s spectral extraction mask to be applied in the scientific data 239s reduction, performed with the recipe fors_science. This recipe accepts 239s both FORS1 and FORS2 frames. The input arc lamp and flat field 239s exposures are assumed to be obtained quasi-simultaneously, so that 239s they would be described by exactly the same instrument distortions. A 239s line catalog must be specified, containing the wavelengths of the 239s reference arc lamp lines used for the wavelength calibration. A grism 239s table (typically depending on the instrument mode, and in particular 239s on the grism used) may also be specified: this table contains a 239s default recipe parameter setting to control the way spectra are 239s extracted for a specific instrument mode, as it is used for automatic 239s run of the pipeline on Paranal and in Garching. If this table is 239s specified, it will modify the default recipe parameter setting, with 239s the exception of those parameters which have been explicitly modified 239s on the command line. If a grism table is not specified, the input 239s recipe parameters values will always be read from the command line, or 239s from an esorex configuration file if present, or from their generic 239s default values (that are rarely meaningful). Finally a master bias 239s frame must be input to this recipe. In the table below the MXU acronym 239s can be read alternatively as MOS and LSS, with the exception of 239s CURV_COEFF_LSS, CURV_TRACES_LSS, SPATIAL_MAP_LSS, 239s SPECTRA_DETECTION_LSS, and and SLIT_MAP_LSS, which are never created. 239s The products SPECTRA_DETECTION_MXU, SLIT_MAP_MXU, and 239s DISP_RESIDUALS_MXU, are just created if the --check parameter is set 239s to true. The product GLOBAL_DISTORTION_TABLE is just created if more 239s than 12 separate spectra are found in the CCD. Input files: DO 239s category: Type: Explanation: Required: 239s SCREEN_FLAT_MXU Raw Flat field exposures Y 239s LAMP_MXU Raw Arc lamp exposure Y 239s MASTER_BIAS Calib Master Bias frame Y 239s MASTER_LINECAT Calib Line catalog Y 239s GRISM_TABLE Calib Grism table . Output 239s files: DO category: Data type: Explanation: 239s MASTER_SCREEN_FLAT_MXU FITS image Combined (sum) flat field 239s MASTER_NORM_FLAT_MXU FITS image Normalised flat field 239s MAPPED_SCREEN_FLAT_MXU FITS image Wavelength calibrated flat field 239s MAPPED_NORM_FLAT_MXU FITS image Wavelength calibrated normalised 239s flat REDUCED_LAMP_MXU FITS image Wavelength calibrated arc 239s spectrum DISP_COEFF_MXU FITS table Inverse dispersion 239s coefficients DISP_RESIDUALS_MXU FITS image Residuals in 239s wavelength calibration DISP_RESIDUALS_TABLE_MXU FITS table 239s Residuals in wavelength calibration DELTA_IMAGE_MXU FITS 239s image Offset vs linear wavelength calib WAVELENGTH_MAP_MXU 239s FITS image Wavelength for each pixel on CCD SPECTRA_DETECTION_MXU 239s FITS image Check for preliminary detection SLIT_MAP_MXU 239s FITS image Map of central wavelength on CCD CURV_TRACES_MXU 239s FITS table Spectral curvature traces CURV_COEFF_MXU FITS 239s table Spectral curvature coefficients SPATIAL_MAP_MXU FITS 239s image Spatial position along slit on CCD SPECTRAL_RESOLUTION_MXU 239s FITS table Resolution at reference arc lines DETECTED_LINES_MXU 239s FITS table All the lines detected in the arc ARC_RECTIFIED_MXU 239s FITS image The spatial rectified arc SLIT_LOCATION_MXU FITS 239s table Slits on product frames and CCD GLOBAL_DISTORTION_TABLE FITS 239s table Global distortions table FLAT_SED_LSS FITS image 239s Average SED for each of the slitsi 239s 239s Parameters: 239s dispersion: Expected spectral dispersion (Angstrom/pixel) 239s (float; default: 0.0) 239s peakdetection: Initial peak detection threshold (ADU) (float; 239s default: 0.0) 239s wdegree: Degree of wavelength calibration polynomial 239s (int; default: 0) 239s wradius: Search radius if iterating pattern-matching with 239s first-guess method (int; default: 4) 239s wreject: Rejection threshold in dispersion relation fit 239s (pixel) (float; default: 0.7) 239s wmode: Interpolation mode of wavelength solution 239s applicable to LSS-like data (0 = no 239s interpolation, 1 = fill gaps, 2 = global model) 239s (int; default: 2) 239s wmosmode: Interpolation mode of wavelength solution (0 = 239s no interpolation, 1 = local (slit) solution, 2 = 239s global model) (int; default: 0) 239s ignore_lines: Catalog lines nearest to wavelengths in this 239s list will be ignored for wavelength calibration 239s (str; default: '') 239s used_linesets: Linesets to use. Valid are 'standard' 239s and'extended' (see column LINE_SET in the line 239s catalogue) (str; default: 'standard') 239s cdegree: Degree of spectral curvature polynomial (int; 239s default: -1) 239s cmode: Interpolation mode of curvature solution 239s applicable to MOS-like data (0 = no 239s interpolation, 1 = fill gaps, 2 = global model) 239s (int; default: 1) 239s startwavelength: Start wavelength in spectral extraction (float; 239s default: 0.0) 239s endwavelength: End wavelength in spectral extraction (float; 239s default: 0.0) 239s slit_ident: Attempt slit identification for MOS or MXU 239s (bool; default: False) 239s stack_method: Frames combination method (str; default: 'sum') 239s ksigma: Low and high threshold in ksigma method (str; 239s default: '-3.0,3.0') 239s kiter: Max number of iterations in ksigma method (int; 239s default: 999) 239s s_degree: Polynomial degree for the flat field fitting 239s along spatial direction (int; default: -1) 239s sradius: Smooth box radius for flat field along spatial 239s direction (int; default: -1) 239s d_nknots: Number of knots in flat field fitting splines 239s along dispersion direction (int; default: -1) 239s dradius: Smooth box radius (median) for flat field along 239s dispersion direction (int; default: 10) 239s dradius_aver: Smooth box radius (average) for flat field along 239s dispersion direction (performed after median 239s smoothing) (int; default: -1) 239s fit_threshold: Threshold percentage for flat spline fittingwith 239s respect to the maximum (float; default: 0.01) 239s nonlinear_level: Level above which the detector is not linear 239s (float; default: 60000.0) 239s max_nonlinear_ratio: Maximum allowed ratio of non-linear pixels per 239s slit (float; default: 0.2) 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_align_sky_lss: 239s version 5.5.7 239s Parameters: {'dispersion': 0.0, 'startwavelength': 0.0, 'endwavelength': 0.0, 'skyalign': 0, 'wcolumn': 'WLEN'} 239s Docstring: Upgrade wavelength solution using sky lines 239s 239s This recipe is used to align the wavelength solution based on the arc 239s lamp exposure on a set of sky lines observed on a scientific exposure. 239s The input scientific frames are produced by the recipes 239s fors_remove_bias and fors_flatfield. An input catalog of sky lines can 239s be specified, or an internal one is used. This recipe should be 239s applied to LSS or long-slit like data (MOS/MXU with all slits at the 239s same offset). For multi-slit MOS/MXU data use recipe fors_align_sky 239s instead. Please refer to the FORS PIpeline User's Manual for more 239s details. In the table below the MXU acronym can be alternatively read 239s as MOS and LSS, and SCI as STD. Input files: DO category: 239s Type: Explanation: Required: SCIENCE_UNBIAS_MXU or 239s SCIENCE_UNFLAT_MXU or STANDARD_UNBIAS_MXU or STANDARD_UNFLAT_MXU 239s Calib Frame with sky lines Y DISP_COEFF_MXU 239s Calib Dispersion solution Y SLIT_LOCATION_MXU 239s Calib Slit location on CCD Y MASTER_SKYLINECAT 239s Calib Catalog of sky lines . GRISM_TABLE 239s Calib Grism table . Output files: DO category: 239s Data type: Explanation: SKY_SHIFTS_LONG_SCI_MXU FITS table 239s Observed sky lines offsets WAVELENGTH_MAP_SCI_MXU FITS image 239s Wavelength mapped on CCD DISP_COEFF_SCI_MXU FITS image 239s Upgraded dispersion solution 239s 239s Parameters: 239s dispersion: Expected spectral dispersion (Angstrom/pixel) 239s (float; default: 0.0) 239s startwavelength: Start wavelength in spectral extraction (float; 239s default: 0.0) 239s endwavelength: End wavelength in spectral extraction (float; 239s default: 0.0) 239s skyalign: Polynomial order for sky lines alignment (int; 239s default: 0) 239s wcolumn: Name of sky line catalog table column with 239s wavelengths (str; default: 'WLEN') 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_wave_calib_lss: 239s version 5.5.7 239s Parameters: {'dispersion': 0.0, 'peakdetection': 0.0, 'wdegree': 0, 'wradius': 4, 'wreject': 0.7, 'wcolumn': 'WLEN', 'startwavelength': 0.0, 'endwavelength': 0.0, 'wmode': 2} 239s Docstring: Derive dispersion relation from long-slit arc lamp frame 239s 239s This recipe is used to wavelength calibrate one long slit spectrum, 239s i.e., a FORS spectral obtained either in LSS mode or in MOS/MXU mode 239s with all slits at the same offset. A pattern-matching algorithm is 239s applied as in recipe fors_detect_spectra. For more details on this 239s data reduction strategy please refer to the FORS Pipeline User's 239s Manual. Note that specifying an input GRISM_TABLE will set some of 239s the recipe configuration parameters to default values valid for a 239s particular grism. In the table below the LSS acronym can be 239s alternatively read as MOS or MXU. Input files: DO category: 239s Type: Explanation: Required: LAMP_UNBIAS_LSS 239s Calib Arc lamp exposure Y MASTER_LINECAT 239s Calib Line catalog Y GRISM_TABLE 239s Calib Grism table . Output files: DO category: 239s Data type: Explanation: REDUCED_LAMP_LSS FITS image 239s Calibrated arc lamp exposure DISP_COEFF_LSS FITS table 239s Inverse dispersion coefficients DISP_RESIDUALS_LSS FITS 239s image Image of modeling residuals WAVELENGTH_MAP_LSS FITS 239s image Wavelengths mapped on CCD SLIT_LOCATION_LSS FITS 239s image Background subtracted arc frame SPECTRAL_RESOLUTION_LSS 239s FITS table Spectral resolution table 239s 239s Parameters: 239s dispersion: Expected spectral dispersion (Angstrom/pixel) 239s (float; default: 0.0) 239s peakdetection: Initial peak detection threshold (ADU) (float; 239s default: 0.0) 239s wdegree: Degree of wavelength calibration polynomial (int; 239s default: 0) 239s wradius: Search radius if iterating pattern-matching with 239s first-guess method (int; default: 4) 239s wreject: Rejection threshold in dispersion relation fit 239s (pixel) (float; default: 0.7) 239s wcolumn: Name of line catalog table column with wavelengths 239s (str; default: 'WLEN') 239s startwavelength: Start wavelength in spectral extraction (float; 239s default: 0.0) 239s endwavelength: End wavelength in spectral extraction (float; 239s default: 0.0) 239s wmode: Interpolation mode of wavelength solution (0 = no 239s interpolation, 1 = fill gaps, 2 = global model) 239s (int; default: 2) 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_img_science: 239s version 5.5.7 239s 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} 239s Docstring: Reduce imaging scientific exposure 239s 239s Input files: DO category: Type: Explanation: 239s Number: SCIENCE_IMG Raw Science image 239s 1 MASTER_BIAS FITS image Master bias 239s 1 MASTER_SKY_FLAT_IMG FITS image Master sky flat field 239s 1 PHOT_COEFF_TABLE FITS table Observed extinction 239s coefficients 0+ EXTINCTION_PER_NIGHT FITS table 239s Extinction per night 0+ 239s STATIC_PHOT_COEFF_TABLE FITS table Static filters photometry 239s coefficients 0+ DETECTOR_ILLUMINATED_REGION FITS table 239s Table with detector illuminated regions 0+ Output files: DO 239s category: Data type: Explanation: SCIENCE_REDUCED_IMG 239s FITS image Reduced science image PHOT_BACKGROUND_SCI_IMG FITS 239s image Reduced science image background SOURCES_SCI_IMG 239s FITS image Unfiltered SExtractor output OBJECT_TABLE_SCI_IMG 239s FITS table Extracted sources properties SCIENCE_REDUCED_IMG_IDP 239s FITS image Reduced science image in IDP-compliant format 239s SCIENCE_REDUCED_WEIGHT_IDP FITS image Ancillary file with the weights 239s for IDP the image SCIENCE_REDUCED_ERR_IDP FITS image Ancillary 239s file with the errors for IDP the image 239s 239s Parameters: 239s magsyserr: Systematic error in magnitude (float; default: 239s 0.01) 239s sex_exe: SExtractor executable (str; default: 239s '/usr/bin/source-extractor') 239s sex_config: SExtractor configuration file (str; default: 239s '/usr/share/cpl- 239s plugins/fors-5.5.7/config/fors.sex') 239s sex_mag: SExtractor magnitude (str; default: 239s 'MAG_APER') 239s sex_magerr: SExtractor magnitude error (str; default: 239s 'MAGERR_APER') 239s sex_radius: Background error map median filter radius 239s (unbinned pixels) (int; default: 64) 239s idp_generate: If TRUE compliant IDP science products are 239s generated (bool; default: False) 239s idp_weights_threshold: Every pixel in the MASTER_SKY_FLAT_IMG below 239s the threshold will be put to 0 in the weight- 239s map, 1 otherwise. Ignored if IDP generation is 239s not requested (float; default: 0.5) 239s Author: ESO PPS Group 239s 239s 239s Recipe fors_extract_objects: 239s version 5.5.7 239s Parameters: {'ext_mode': 1} 239s Docstring: Extract objects in slit spectra 239s 239s This recipe is used to extract scientific objects spectra on a 239s resampled image produced with recipe fors_resample, at the positions 239s listed in the object table produced by recipe fors_detect_objects. 239s Please refer to the FORS Pipeline User's Manual for more details on 239s object extraction. In the table below the MXU acronym can be 239s alternatively read as MOS and LSS, and SCI as STD. Input files: DO 239s category: Type: Explanation: Required: 239s MAPPED_SCI_MXU Calib Resampled slit spectra Y 239s MAPPED_SKY_SCI_MXU Calib Resampled sky spectra Y 239s OBJECT_TABLE_SCI_MXU Calib Object table Y 239s Output files: DO category: Data type: Explanation: 239s REDUCED_SCI_MXU FITS image Extracted object spectra 239s REDUCED_SKY_SCI_MXU FITS image Extracted sky spectra 239s REDUCED_ERROR_SCI_MXU FITS image Error on extracted spectra 239s 239s Parameters: 239s ext_mode: Object extraction method: 0 = aperture, 1 = Horne optimal 239s extraction (int; default: 1) 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_trace_flat: 239s version 5.5.7 239s Parameters: {'dispersion': 0.0, 'startwavelength': 0.0, 'endwavelength': 0.0, 'cdegree': 0, 'cmode': 1} 239s Docstring: Determine spectral curvature model 239s 239s This recipe is used to trace the edges of MOS/MXU flat field slit 239s spectra and determine the spectral curvature solution. The input 239s master flat field image, product of the recipe fors_flat, is expected 239s to be oriented with horizontal dispersion direction and red 239s wavelengths on the right side. The input slits location table should 239s be the product of the recipe fors_detect_spectra. The input master 239s flat image is shifted one pixel down and is subtracted from the 239s original image. The result is a vertical gradient map. Next, the 239s negative values are forced positive, to obtain an absolute gradient 239s map. The map is passed with a horizontal median filter, and after that 239s the gradient peaks are traced starting from the slits positions listed 239s in the input slits location table. The number of pixels to the left 239s and to the right of the reference pixel is trivially derived from the 239s specified spectral range and spectral dispersion. The output spectral 239s curvature table contains the coefficients of the polynomial fitting of 239s the found traces, while the output trace table contains the traced 239s spectral edges positions in CCD (Y) coordinates for each spectrum, and 239s their comparison with their modeling. A spatial map is also created, 239s where to each CCD pixel is assigned the value of the spatial 239s coordinate along the slit (in pixel). For more details please refer to 239s the FORS Pipeline User's Manual. Note that specifying an input 239s GRISM_TABLE will set some of the recipe configuration parameters to 239s default values valid for a particular grism. Again, see the pipeline 239s manual for more details. In the table below the MXU acronym can be 239s alternatively read as MOS. Input files: DO category: 239s Type: Explanation: Required: MASTER_SCREEN_FLAT_MXU 239s Calib Master flat frame Y SLIT_LOCATION_DETECT_MXU 239s Calib Slits location Y GRISM_TABLE 239s Calib Grism table . Output files: DO category: 239s Data type: Explanation: CURV_TRACES_MXU FITS table Flat 239s field tracings CURV_COEFF_MXU FITS table Spectral 239s curvature table SPATIAL_MAP_MXU FITS image Map of 239s spatial coordinate 239s 239s Parameters: 239s dispersion: Expected spectral dispersion (Angstrom/pixel) 239s (float; default: 0.0) 239s startwavelength: Start wavelength in spectral extraction (float; 239s default: 0.0) 239s endwavelength: End wavelength in spectral extraction (float; 239s default: 0.0) 239s cdegree: Degree of spectral curvature polynomial (int; 239s default: 0) 239s cmode: Interpolation mode of curvature solution applicable 239s to MOS-like data (0 = no interpolation, 1 = fill 239s gaps, 2 = global model) (int; default: 1) 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_remove_bias: 239s version 5.5.7 239s Parameters: {} 239s Docstring: Subtract bias from input frame 239s 239s This recipe is used to subtract the overscan and master bias(produced 239s by the recipe fors_bias) from one raw data frame. The overscan 239s regions, if present, are used to compensate for variations of the 239s overall bias level between master bias and input raw frame. The 239s overscan regions are then trimmed from the result. The recipe should 239s allow any fors frame. Input files: DO category: 239s Type: Explanation: Required: ANY_CAT 239s Raw Raw data frame Y MASTER_BIAS 239s Calib Master bias frame Y Output files: DO category: 239s Data type: Explanation: ANY_CAT_UNBIAS FITS image Bias 239s subtracted frame 239s 239s No parameters 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_pmos_extract: 239s version 5.5.7 239s 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} 239s Docstring: Extraction of scientific spectra 239s 239s This recipe is used to reduce scientific spectra using the extraction 239s mask and the products created by the recipe fors_mpol_calib. The 239s spectra are bias subtracted, flat fielded (if a normalised flat field 239s is specified) and remapped eliminating the optical distortions. The 239s wavelength calibration can be optionally upgraded using a number of 239s sky lines: if no sky lines catalog of wavelengths is specified, an 239s internal one is used instead. If the alignment to the sky lines is 239s performed, the input dispersion coefficients table is upgraded and 239s saved to disk, and a new CCD wavelengths map is created. This recipe 239s accepts both FORS1 and FORS2 frames. A grism table (typically 239s depending on the instrument mode, and in particular on the grism used) 239s may also be specified: this table contains a default recipe parameter 239s setting to control the way spectra are extracted for a specific 239s instrument mode, as it is used for automatic run of the pipeline on 239s Paranal and in Garching. If this table is specified, it will modify 239s the default recipe parameter setting, with the exception of those 239s parameters which have been explicitly modifyed on the command line. If 239s a grism table is not specified, the input recipe parameters values 239s will always be read from the command line, or from an esorex 239s configuration file if present, or from their generic default values 239s (that are rarely meaningful). Either a scientific or a standard star 239s exposure can be specified in input. The acronym SCI on products should 239s be read STD in case of standard stars observations. Input files: 239s DO category: Type: Explanation: Required: 239s SCIENCE_PMOS Raw Scientific exposure Y 239s or STANDARD_PMOS Raw Standard star exposure Y 239s MASTER_BIAS Calib Master bias Y 239s GRISM_TABLE Calib Grism table . 239s MASTER_SKYLINECAT Calib Sky lines catalog . 239s MASTER_NORM_FLAT_PMOS Calib Normalised flat field . 239s DISP_COEFF_PMOS Calib Inverse dispersion Y 239s CURV_COEFF_PMOS Calib Spectral curvature Y 239s SLIT_LOCATION_PMOS Calib Slits positions table Y 239s RETARDER_WAVEPLATE_CHROMATISM Calib Chromatism correction . 239s Output files: DO category: Data type: Explanation: 239s REDUCED_SCI_PMOS FITS image Extracted scientific spectra 239s REDUCED_SKY_SCI_PMOS FITS image Extracted sky spectra 239s REDUCED_ERROR_SCI_PMOS FITS image Errors on extracted spectra 239s REDUCED_SCI_X_PMOS FITS image X Stokes parameter (and L) 239s REDUCED_ERROR_X_PMOS FITS image Error on X Stokes parameter 239s REDUCED_NUL_X_PMOS FITS image Null parameter for X 239s REDUCED_POL_ANGLE_PMOS FITS image Direction of linear 239s polarization REDUCED_POL_ANGLE_ERROR_PMOS FITS image Error on 239s polarization direction UNMAPPED_SCI_PMOS FITS image Sky 239s subtracted scientific spectra MAPPED_SCI_PMOS FITS 239s image Rectified scientific spectra MAPPED_ALL_SCI_PMOS 239s FITS image Rectified science spectra with sky MAPPED_SKY_SCI_PMOS 239s FITS image Rectified sky spectra UNMAPPED_SKY_SCI_PMOS FITS 239s image Sky on CCD GLOBAL_SKY_SPECTRUM_PMOS FITS table Global 239s sky spectrum OBJECT_TABLE_SCI_PMOS FITS table Positions of 239s detected objects OBJECT_TABLE_POL_SCI_PMOS FITS table Positions 239s of real objects Only if the sky-alignment of the wavelength 239s solution is requested: DISP_COEFF_SCI_PMOS FITS table 239s Upgraded dispersion coefficients WAVELENGTH_MAP_SCI_PMOS FITS 239s image Upgraded wavelength map 239s 239s Parameters: 239s dispersion: Resampling step (Angstrom/pixel) (float; default: 239s 0.0) 239s skyalign: Polynomial order for sky lines alignment, or -1 to 239s avoid alignment (int; default: 0) 239s wcolumn: Name of sky line catalog table column with 239s wavelengths (str; default: 'WLEN') 239s startwavelength: Start wavelength in spectral extraction (float; 239s default: 0.0) 239s endwavelength: End wavelength in spectral extraction (float; 239s default: 0.0) 239s flux: Apply flux conservation (bool; default: True) 239s flatfield: Apply flat field (bool; default: False) 239s skyglobal: Subtract global sky spectrum from CCD (bool; 239s default: False) 239s skymedian: Sky subtraction from extracted slit spectra (bool; 239s default: False) 239s skylocal: Sky subtraction from CCD slit spectra (bool; 239s default: True) 239s cosmics: Eliminate cosmic rays hits (only if global sky 239s subtraction is also requested) (bool; default: 239s False) 239s slit_margin: Number of pixels to exclude at each slit in object 239s detection and extraction (int; default: 3) 239s ext_radius: Maximum extraction radius for detected objects 239s (pixel) (int; default: 6) 239s cont_radius: Minimum distance at which two objects of equal 239s luminosity do not contaminate each other (pixel) 239s (int; default: 0) 239s ext_mode: Object extraction method: 0 = aperture, 1 = Horne 239s optimal extraction (int; default: 1) 239s time_normalise: Normalise output spectra by the exposure time (bool; 239s default: True) 239s chromatism: Chromatism correction to polarization angles (bool; 239s default: True) 239s check: Create intermediate products (bool; default: False) 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_pmos_calib: 239s version 5.5.7 239s 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} 239s Docstring: Determination of the extraction mask 239s 239s This recipe is used to identify reference lines on PMOS arc lamp 239s exposures, and trace the spectral edges on the corresponding flat 239s field exposures. This information is used to determine the spectral 239s extraction mask to be applied in the scientific data reduction, 239s performed with the recipe fors_science. This recipe accepts both FORS1 239s and FORS2 frames. The input arc lamps and flat field exposures are 239s assumed to be obtained quasi-simultaneously, so that they would be 239s described by exactly the same instrument distortions. A line catalog 239s must be specified, containing the wavelengths of the reference arc 239s lamp lines used for the wavelength calibration. A grism table 239s (typically depending on the instrument mode, and in particular on the 239s grism used) may also be specified: this table contains a default 239s recipe parameter setting to control the way spectra are extracted for 239s a specific instrument mode, as it is used for automatic run of the 239s pipeline on Paranal and in Garching. If this table is specified, it 239s will modify the default recipe parameter setting, with the exception 239s of those parameters which have been explicitly modifyed on the command 239s line. If a grism table is not specified, the input recipe parameters 239s values will always be read from the command line, or from an esorex 239s configuration file if present, or from their generic default values 239s (that are rarely meaningful). Finally a master bias frame must be 239s input to this recipe. The products SPECTRA_DETECTION_PMOS, 239s SLIT_MAP_PMOS, and DISP_RESIDUALS_PMOS, are just created if the 239s --check parameter is set to true. The MASTER_DISTORTION_TABLE is 239s marked as required, but it is not so if all slits have different 239s offsets, and in the case of FORS1 observations made with the old 239s TK2048EB4-1 1604 chip read in windowed mode (2048x400) Input files: 239s DO category: Type: Explanation: Required: 239s SCREEN_FLAT_PMOS Raw Flat field exposures Y 239s LAMP_PMOS Raw Arc lamp exposure Y 239s MASTER_BIAS or BIAS Calib Bias frame Y 239s MASTER_LINECAT Calib Line catalog Y 239s GRISM_TABLE Calib Grism table . 239s MASTER_DISTORTION_TABLE Calib Master distortions table Y 239s Output files: DO category: Data type: Explanation: 239s MASTER_SCREEN_FLAT_PMOS FITS image Combined (sum) flat field 239s MASTER_NORM_FLAT_PMOS FITS image Normalised flat field 239s MAPPED_SCREEN_FLAT_PMOS FITS image Wavelength calibrated flat field 239s MAPPED_NORM_FLAT_PMOS FITS image Wavelength calibrated normalised 239s flat REDUCED_LAMP_PMOS FITS image Wavelength calibrated arc 239s spectrum DISP_COEFF_PMOS FITS table Inverse dispersion 239s coefficients DISP_RESIDUALS_PMOS FITS image Residuals in 239s wavelength calibration DISP_RESIDUALS_TABLE_PMOS FITS table 239s Residuals in wavelength calibration DELTA_IMAGE_PMOS FITS 239s image Offset vs linear wavelength calib WAVELENGTH_MAP_PMOS 239s FITS image Wavelength for each pixel on CCD SPECTRA_DETECTION_PMOS 239s FITS image Check for preliminary detection SLIT_MAP_PMOS 239s FITS image Map of central wavelength on CCD CURV_TRACES_PMOS 239s FITS table Spectral curvature traces CURV_COEFF_PMOS FITS 239s table Spectral curvature coefficients SPATIAL_MAP_PMOS 239s FITS image Spatial position along slit on CCD 239s SPECTRAL_RESOLUTION_PMOS FITS table Resolution at reference arc 239s lines SLIT_LOCATION_PMOS FITS table Slits on product frames 239s and CCD 239s 239s Parameters: 239s dispersion: Expected spectral dispersion (Angstrom/pixel) 239s (float; default: 0.0) 239s peakdetection: Initial peak detection threshold (ADU) (float; 239s default: 0.0) 239s wdegree: Degree of wavelength calibration polynomial (int; 239s default: 0) 239s wradius: Search radius if iterating pattern-matching with 239s first-guess method (int; default: 4) 239s wreject: Rejection threshold in dispersion relation fit 239s (pixel) (float; default: 0.7) 239s wcolumn: Name of line catalog table column with wavelengths 239s (str; default: 'WLEN') 239s cdegree: Degree of spectral curvature polynomial (int; 239s default: 0) 239s cmode: Interpolation mode of curvature solution (0 = no 239s interpolation, 1 = fill gaps, 2 = global model) 239s (int; default: 1) 239s startwavelength: Start wavelength in spectral extraction (float; 239s default: 0.0) 239s endwavelength: End wavelength in spectral extraction (float; 239s default: 0.0) 239s stack_method: Frames combination method (str; default: 'average') 239s minrejection: Number of lowest values to be rejected (int; 239s default: 1) 239s maxrejection: Number of highest values to be rejected (int; 239s default: 1) 239s klow: Low threshold in ksigma method (float; default: 3.0) 239s khigh: High threshold in ksigma method (float; default: 239s 3.0) 239s kiter: Max number of iterations in ksigma method (int; 239s default: 999) 239s ddegree: Degree of flat field fitting polynomial along 239s dispersion direction (int; default: -1) 239s dradius: Smooth box radius for flat field along dispersion 239s direction (int; default: 10) 239s qc: Compute QC1 parameters (bool; default: True) 239s check: Create intermediate products (bool; default: False) 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_align_sky: 239s version 5.5.7 239s Parameters: {'dispersion': 0.0, 'startwavelength': 0.0, 'endwavelength': 0.0, 'skyalign': 0, 'wcolumn': 'WLEN'} 239s Docstring: Upgrade wavelength solution using sky lines 239s 239s This recipe is used to align the wavelength solution based on the arc 239s lamp exposure on a set of sky lines observed on a scientific exposure. 239s The input rectified frames are produced by the recipe 239s fors_extract_slits. An input catalog of sky lines can be specified, 239s otherwise an internal one is used. This recipe should be applied to 239s multi-slit MOS/MXU data: for LSS or long-slit like data (MOS/MXU with 239s all slits at the same offset) use recipe fors_align_sky_lss instead. 239s Please refer to the FORS Pipeline User's Manual for more details. In 239s the table below the MXU acronym can be alternatively read as MOS, and 239s SCI as STD. Input files: DO category: Type: 239s Explanation: Required: RECTIFIED_ALL_SCI_MXU or 239s RECTIFIED_SKY_SCI_MXU Calib Frame with sky lines Y 239s SPATIAL_MAP_MXU Calib Spatial coordinate map Y 239s CURV_COEFF_MXU Calib Spectral curvature Y 239s SLIT_LOCATION_MXU Calib Slit location on CCD Y 239s DISP_COEFF_MXU Calib Dispersion solution Y 239s MASTER_SKYLINECAT Calib Catalog of sky lines . 239s GRISM_TABLE Calib Grism table . 239s Output files: DO category: Data type: Explanation: 239s SKY_SHIFTS_SLIT_SCI_MXU FITS table Observed sky lines offsets 239s WAVELENGTH_MAP_SCI_MXU FITS image Wavelength mapped on CCD 239s DISP_COEFF_SCI_MXU FITS image Upgraded dispersion solution 239s 239s Parameters: 239s dispersion: Expected spectral dispersion (Angstrom/pixel) 239s (float; default: 0.0) 239s startwavelength: Start wavelength in spectral extraction (float; 239s default: 0.0) 239s endwavelength: End wavelength in spectral extraction (float; 239s default: 0.0) 239s skyalign: Polynomial order for sky lines alignment (int; 239s default: 0) 239s wcolumn: Name of sky line catalog table column with 239s wavelengths (str; default: 'WLEN') 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_normalise_flat: 239s version 5.5.7 239s 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} 239s Docstring: Normalise master flat spectrum 239s 239s This recipe is used to normalise a master flat field frame dividing it 239s by its large scale illumination trend. This recipe can be applied both 239s to generic multi-slit (MOS/MXU) and to long slit exposures (either 239s LSS, or LSS-like MOS/MXU), even if different normalisation methods are 239s applied in such different cases. The input master flat field image is 239s the product of the recipe fors_flat. The input spectral curvature 239s table, product of the recipe fors_detect_spectra, is only required in 239s the case of multi-slit data. In the case of multi-slit data, the flat 239s field spectra are spatially rectified, heavily smoothed, and then 239s mapped back on the CCD. Then the master flat image is divided by its 239s smoothed counterpart. The smoothing may be obtained either by applying 239s a running median filter of specified sizes, or by polynomial fitting 239s along the dispersion direction performed independently for each row of 239s the spatially remapped spectra. In the case of long-slit data, the 239s smoothing can still be obtained either by applying a running median 239s filter or by polynomial fitting, but the polynomial fitting will be 239s performed along the spatial direction, for each column of the 239s spectrum. In the table below the MXU acronym can be alternatively 239s read as MOS or LSS. Input files: DO category: Type: 239s Explanation: Required: MASTER_SCREEN_FLAT_MXU Calib 239s Master flat frame Y DISP_COEFF_MXU Calib 239s Wavelength calibration Y CURV_COEFF_MXU Calib 239s Spectral curvature . SLIT_LOCATION_MXU Calib 239s Slit detection . GRISM_TABLE Calib 239s Grism table Y Output files: DO category: 239s Data type: Explanation: MASTER_NORM_FLAT_MXU FITS image 239s Normalised flat field 239s 239s Parameters: 239s dispersion: Expected spectral dispersion (Angstrom/pixel) 239s (float; default: 0.0) 239s startwavelength: Start wavelength in spectral extraction (float; 239s default: 0.0) 239s endwavelength: End wavelength in spectral extraction (float; 239s default: 0.0) 239s spa_polydegree: Polynomial degree for the flat field fitting along 239s spatial direction (int; default: -1) 239s sradius: Smooth box radius for flat field along spatial 239s direction (int; default: 10) 239s disp_nknots: Number of knots in flat field fitting splines along 239s dispersion direction (int; default: -1) 239s dradius: Smooth box radius (median) for flat field along 239s dispersion direction (int; default: 10) 239s dradius_aver: Smooth box radius (average) for flat field along 239s dispersion direction (performed after median 239s smoothing) (int; default: 10) 239s splfit_threshold: Threshold percentage for flat spline fittingwith 239s respect to the maximum (float; default: 0.01) 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_dark: 239s version 5.5.7 239s Parameters: {'stack_method': 'median', 'minrejection': 1, 'maxrejection': 1, 'klow': 3.0, 'khigh': 3.0, 'kiter': 999} 239s Docstring: Compute master dark frame 239s 239s This recipe is used to combine input raw DARK frames into a master 239s dark frame by subtracing the master bias and using the given stacking 239s method. The overscan regions, if present, are removed from the result. 239s Input files: DO category: Type: Explanation: 239s Required: DARK Raw Dark frame 239s Y MASTER_BIAS FITS image Master bias Y 239s Output files: DO category: Data type: Explanation: 239s MASTER_DARK FITS image Master dark frame 239s 239s Parameters: 239s stack_method: Frames combination method (str; default: 'median') 239s minrejection: Number of lowest values to be rejected (int; default: 239s 1) 239s maxrejection: Number of highest values to be rejected (int; default: 239s 1) 239s klow: Low threshold in ksigma method (float; default: 3.0) 239s khigh: High threshold in ksigma method (float; default: 3.0) 239s kiter: Max number of iterations in ksigma method (int; 239s default: 999) 239s Author: Jonas M. Larsen 239s 239s 239s Recipe fors_detect_objects: 239s version 5.5.7 239s Parameters: {'slit_margin': 3, 'ext_radius': 6, 'cont_radius': 0} 239s Docstring: Detect objects in slit spectra 239s 239s This recipe is used to detect scientific objects spectra on a 239s resampled image produced with recipe fors_resample. Please refer to 239s the FORS Pipeline User's Manual for more details on object detection. 239s In the table below the MXU acronym can be alternatively read as MOS 239s and LSS, and SCI as STD. Input files: DO category: 239s Type: Explanation: Required: MAPPED_SCI_MXU 239s Calib Resampled slit spectra Y SLIT_LOCATION_MXU 239s Calib Slit location on image Y Output files: DO category: 239s Data type: Explanation: OBJECT_TABLE_SCI_MXU FITS table 239s Object positions in slit spectra 239s 239s Parameters: 239s slit_margin: Number of pixels to exclude at each slit in object 239s detection and extraction (int; default: 3) 239s ext_radius: Maximum extraction radius for detected objects (pixel) 239s (int; default: 6) 239s cont_radius: Minimum distance at which two objects of equal 239s luminosity do not contaminate each other (pixel) (int; 239s default: 0) 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_extract: 239s version 5.5.7 239s 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} 239s Docstring: Extraction of scientific spectra 239s 239s This recipe is used to reduce scientific spectra using the global 239s distortion table created by the recipe fors_calib. The spectra are 239s bias subtracted, flat fielded (if a normalised flat field is 239s specified) and remapped eliminating the optical distortions. The 239s wavelength calibration can be optionally upgraded using a number of 239s sky lines: if no sky lines catalog of wavelengths is specified, an 239s internal one is used instead. If the alignment to the sky lines is 239s performed, the applied dispersion coefficient table is upgraded and 239s saved to disk, and a new CCD wavelengths map is created. This recipe 239s accepts both FORS1 and FORS2 frames. A grism table (typically 239s depending on the instrument mode, and in particular on the grism used) 239s may also be specified: this table contains a default recipe parameter 239s setting to control the way spectra are extracted for a specific 239s instrument mode, as it is used for automatic run of the pipeline on 239s Paranal and in Garching. If this table is specified, it will modify 239s the default recipe parameter setting, with the exception of those 239s parameters which have been explicitly modifyed on the command line. If 239s a grism table is not specified, the input recipe parameters values 239s will always be read from the command line, or from an esorex 239s configuration file if present, or from their generic default values 239s (that are rarely meaningful). In the table below the MXU acronym can 239s be read alternatively as MOS and LSS, depending on the instrument mode 239s of the input data. Either a scientific or a standard star exposure can 239s be specified in input (not both). Input files: DO category: 239s Type: Explanation: Required: SCIENCE_MXU 239s Raw Scientific exposure Y or STANDARD_MXU Raw 239s Standard star exposure Y MASTER_BIAS Calib 239s Master bias Y GRISM_TABLE Calib 239s Grism table . MASTER_SKYLINECAT Calib Sky 239s lines catalog . MASTER_NORM_FLAT_MXU Calib 239s Normalised flat field . MASTER_DISTORTION_TABLE Calib 239s Global distortion model . or, in case of LSS-like MOS/MXU data, 239s MASTER_NORM_FLAT_LONG_MXU Calib Normalised flat field . 239s Output files: DO category: Data type: Explanation: 239s REDUCED_SCI_MXU FITS image Extracted scientific spectra 239s REDUCED_SKY_SCI_MXU FITS image Extracted sky spectra 239s REDUCED_ERROR_SCI_MXU FITS image Errors on extracted spectra 239s UNMAPPED_SCI_MXU FITS image Sky subtracted scientific 239s spectra MAPPED_SCI_MXU FITS image Rectified scientific 239s spectra MAPPED_ALL_SCI_MXU FITS image Rectified science 239s spectra with sky MAPPED_SKY_SCI_MXU FITS image Rectified 239s sky spectra UNMAPPED_SKY_SCI_MXU FITS image Sky on CCD 239s GLOBAL_SKY_SPECTRUM_MXU FITS table Global sky spectrum 239s OBJECT_TABLE_SCI_MXU FITS table Positions of detected objects 239s Only if the sky-alignment of the wavelength solution is requested: 239s SKY_SHIFTS_LONG_SCI_MXU FITS table Sky lines offsets (LSS-like 239s data) or SKY_SHIFTS_SLIT_SCI_MXU FITS table Sky lines offsets (MOS- 239s like data) DISP_COEFF_SCI_MXU FITS table Upgraded 239s dispersion coefficients WAVELENGTH_MAP_SCI_MXU FITS image 239s Upgraded wavelength map 239s 239s Parameters: 239s dispersion: Resampling step (Angstrom/pixel) (float; default: 239s 0.0) 239s skyalign: Polynomial order for sky lines alignment, or -1 to 239s avoid alignment (int; default: 0) 239s wcolumn: Name of sky line catalog table column with 239s wavelengths (str; default: 'WLEN') 239s startwavelength: Start wavelength in spectral extraction (float; 239s default: 0.0) 239s endwavelength: End wavelength in spectral extraction (float; 239s default: 0.0) 239s flux: Apply flux conservation (bool; default: True) 239s flatfield: Apply flat field (bool; default: False) 239s skyglobal: Subtract global sky spectrum from CCD (bool; 239s default: False) 239s skymedian: Sky subtraction from extracted slit spectra (bool; 239s default: False) 239s skylocal: Sky subtraction from CCD slit spectra (bool; 239s default: True) 239s cosmics: Eliminate cosmic rays hits (only if global sky 239s subtraction is also requested) (bool; default: 239s False) 239s slit_margin: Number of pixels to exclude at each slit in object 239s detection and extraction (int; default: 3) 239s ext_radius: Maximum extraction radius for detected objects 239s (pixel) (int; default: 6) 239s cont_radius: Minimum distance at which two objects of equal 239s luminosity do not contaminate each other (pixel) 239s (int; default: 0) 239s ext_mode: Object extraction method: 0 = aperture, 1 = Horne 239s optimal extraction (int; default: 1) 239s time_normalise: Normalise output spectra by the exposure time (bool; 239s default: True) 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_img_screen_flat: 239s version 5.5.7 239s Parameters: {'stack_method': 'average', 'minrejection': 1, 'maxrejection': 1, 'klow': 3.0, 'khigh': 3.0, 'kiter': 999, 'xradius': 50, 'yradius': 50, 'degree': -1, 'sampling': 100} 239s Docstring: Compute master screen flat frame 239s 239s After bias subtraction, the input flat field frames are combined using 239s the given stack method. The combined frame is finally normalised 239s dividing it by its large scale illumination trend. The large scale 239s trend is obtained by applying a median filter with a large kernel. To 239s avoid boundary effects, the median filter is applied only to the 239s specified region. The overscan regions, if present, are removed from 239s the result. Input files: DO category: Type: 239s Explanation: Required: SCREEN_FLAT_IMG Raw 239s Screen flat field Y MASTER_BIAS Raw Master 239s bias Y Output files: DO category: Data 239s type: Explanation: MASTER_SCREEN_FLAT_IMG FITS image Master 239s screen flat field 239s 239s Parameters: 239s stack_method: Frames combination method (str; default: 'average') 239s minrejection: Number of lowest values to be rejected (int; default: 239s 1) 239s maxrejection: Number of highest values to be rejected (int; default: 239s 1) 239s klow: Low threshold in ksigma method (float; default: 3.0) 239s khigh: High threshold in ksigma method (float; default: 3.0) 239s kiter: Max number of iterations in ksigma method (int; 239s default: 999) 239s xradius: Median filter x radius (unbinned pixels) (int; default: 239s 50) 239s yradius: Median filter y radius (unbinned pixels) (int; default: 239s 50) 239s degree: Degree of fitting polynomial (int; default: -1) 239s sampling: Sampling interval for fitting (int; default: 100) 239s Author: Jonas M. Larsen 239s 239s 239s Recipe fors_spec_mflat: 239s version 5.5.7 239s 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} 239s Docstring: Computes master spectroscopic flat, removing bias first 239s 239s This recipe is used to subtract the master bias, produced by the 239s recipe fors_bias, from a set of raw flat field frames. The input raw 239s frames are summed, the master bias frame is rescaled accordingly, and 239s subtracted from the result. The overscan regions, if present, are used 239s to compensate for variations of the bias level between master bias and 239s input raw frames. The overscan regions are then trimmed from the 239s result. In the table below the MXU acronym can be alternatively read 239s as MOS and LSS. Input files: DO category: Type: 239s Explanation: Required: SCREEN_FLAT_MXU Raw 239s Raw data frame Y SLIT_LOCATION_MXU Calib 239s Slits positions on CCD Y CURV_COEFF_MXU Calib 239s Slits tracing fits Y DISP_COEFF_MXU Calib 239s Wavelength calibration Y MASTER_BIAS Calib 239s Master bias frame Y Output files: DO category: 239s Data type: Explanation: MASTER_SCREEN_FLAT_MXU FITS image Bias 239s subtracted sum frame 239s 239s Parameters: 239s smooth_sed: Smoothing size for each flat sed (float; 239s default: 0.0) 239s stack_method: Frames combination method (str; default: 'sum') 239s klow: Low threshold in ksigma method (float; default: 239s 3.0) 239s khigh: High threshold in ksigma method (float; default: 239s 3.0) 239s kiter: Max number of iterations in ksigma method (int; 239s default: 999) 239s nonlinear_level: Level above which the detector is not linear 239s (float; default: 50000.0) 239s max_nonlinear_ratio: Maximum allowed ratio of non-linear pixels per 239s slit (float; default: 0.2) 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_pmos_science: 239s version 5.5.7 239s 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} 239s Docstring: Extraction of scientific spectra 239s 239s This recipe is used to reduce scientific spectra using the extraction 239s mask and the products created by the recipe fors_mpol_calib. The 239s spectra are bias subtracted, flat fielded (if a normalised flat field 239s is specified) and remapped eliminating the optical distortions. The 239s wavelength calibration can be optionally upgraded using a number of 239s sky lines: if no sky lines catalog of wavelengths is specified, an 239s internal one is used instead. If the alignment to the sky lines is 239s performed, the input dispersion coefficients table is upgraded and 239s saved to disk, and a new CCD wavelengths map is created. This recipe 239s accepts both FORS1 and FORS2 frames. A grism table (typically 239s depending on the instrument mode, and in particular on the grism used) 239s may also be specified: this table contains a default recipe parameter 239s setting to control the way spectra are extracted for a specific 239s instrument mode, as it is used for automatic run of the pipeline on 239s Paranal and in Garching. If this table is specified, it will modify 239s the default recipe parameter setting, with the exception of those 239s parameters which have been explicitly modifyed on the command line. If 239s a grism table is not specified, the input recipe parameters values 239s will always be read from the command line, or from an esorex 239s configuration file if present, or from their generic default values 239s (that are rarely meaningful). Either a scientific or a standard star 239s exposure can be specified in input. The acronym SCI on products should 239s be read STD in case of standard stars observations. Input files: 239s DO category: Type: Explanation: 239s Required: SCIENCE_PMOS Raw Scientific 239s exposure Y or STANDARD_PMOS Raw Standard 239s star exposure Y MASTER_BIAS Calib Master 239s bias Y GRISM_TABLE Calib Grism 239s table . MASTER_SKYLINECAT Calib Sky 239s lines catalog . MASTER_NORM_FLAT_PMOS Calib 239s Normalised flat field . DISP_COEFF_PMOS Calib 239s Inverse dispersion Y CURV_COEFF_PMOS Calib 239s Spectral curvature Y SLIT_LOCATION_PMOS Calib 239s Slits positions table Y RETARDER_WAVEPLATE_CHROMATISM Calib 239s Chromatism correction . STD_PMOS_TABLE Calib 239s Linear pol. of std stars . Output files: DO category: 239s Data type: Explanation: REDUCED_SCI_PMOS FITS image 239s Extracted scientific spectra REDUCED_SKY_SCI_PMOS FITS image 239s Extracted sky spectra REDUCED_ERROR_SCI_PMOS FITS image 239s Errors on extracted spectra REDUCED_X_SCI_PMOS FITS image 239s X Stokes parameter (and L) REDUCED_ERROR_X_SCI_PMOS FITS image 239s Error on X Stokes parameter REDUCED_NUL_X_SCI_PMOS FITS image 239s Null parameter for X REDUCED_ANGLE_SCI_PMOS FITS image 239s Direction of linear polarization REDUCED_ERROR_ANGLE_SCI_PMOS FITS 239s image Error on polarization direction UNMAPPED_SCI_PMOS 239s FITS image Sky subtracted scientific spectra MAPPED_SCI_PMOS 239s FITS image Rectified scientific spectra MAPPED_ALL_SCI_PMOS 239s FITS image Rectified science spectra with sky MAPPED_SKY_SCI_PMOS 239s FITS image Rectified sky spectra UNMAPPED_SKY_SCI_PMOS FITS 239s image Sky on CCD OBJECT_TABLE_SCI_PMOS FITS table Positions 239s of detected objects OBJECT_TABLE_POL_SCI_PMOS FITS table 239s Positions of real objects Only if the sky-alignment of the 239s wavelength solution is requested: DISP_COEFF_SCI_PMOS FITS 239s table Upgraded dispersion coefficients WAVELENGTH_MAP_SCI_PMOS 239s FITS image Upgraded wavelength map 239s 239s Parameters: 239s dispersion: Expected spectral dispersion (Angstrom/pixel) 239s (float; default: 0.0) 239s rebin: Rebin (pixel) (int; default: 1) 239s skyalign: Polynomial order for sky lines alignment, or -1 to 239s avoid alignment (int; default: 0) 239s wcolumn: Name of sky line catalog table column with 239s wavelengths (str; default: 'WLEN') 239s startwavelength: Start wavelength in spectral extraction (float; 239s default: 0.0) 239s endwavelength: End wavelength in spectral extraction (float; 239s default: 0.0) 239s flux: Apply flux conservation (bool; default: True) 239s flatfield: Apply flat field (bool; default: True) 239s skymedian: Sky subtraction from extracted slit spectra (bool; 239s default: False) 239s skylocal: Sky subtraction from CCD slit spectra (bool; 239s default: True) 239s cosmics: Eliminate cosmic rays hits (only if local sky 239s subtraction is also requested) (bool; default: 239s False) 239s slit_margin: Number of pixels to exclude at each slit in object 239s detection and extraction (int; default: 3) 239s ext_radius: Maximum extraction radius for detected objects 239s (pixel) (int; default: 12) 239s cont_radius: Minimum distance at which two objects of equal 239s luminosity do not contaminate each other (pixel) 239s (int; default: 0) 239s ext_mode: Object extraction method: 0 = aperture, 1 = Horne 239s optimal extraction (int; default: 1) 239s match_tolerance: Tolerance for matching spectra from the same object 239s at different angles and beams (pixel) (float; 239s default: 5.0) 239s time_normalise: Normalise output spectra by the exposure time (bool; 239s default: True) 239s chromatism: Chromatism correction to polarization angles (bool; 239s default: True) 239s wollaston: Wollaston mounting (FORS2 only): true = 0 degrees 239s (ord. beam on top, extr. beam on bottom), false = 239s 180 degrees (beams are reversed), for FORS1 is 239s frozen to true (bool; default: True) 239s qc: Compute QC1 parameters (bool; default: True) 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_subtract_sky_lss: 239s version 5.5.7 239s Parameters: {} 239s Docstring: Subtract sky from calibrated long slit exposure 239s 239s This recipe is used to subtract the sky from wavelength calibrated 239s scientific spectra produced by the recipe fors_resample. A simple 239s median signal level is subtracted from each image column. In the table 239s below the MXU acronym can be read alternatively as MOS and LSS, 239s depending on the instrument mode of the input data. The acronym SCI 239s may be read STD in case of standard stars observations. Note that only 239s LSS or LSS-like MOS/MXU data are to be processed by this recipe. 239s Input files: DO category: Type: Explanation: 239s Required: MAPPED_ALL_SCI_MXU Raw Scientific exposure 239s Y Output files: DO category: Data type: 239s Explanation: MAPPED_SCI_MXU FITS image Rectified 239s scientific spectra MAPPED_SKY_SCI_MXU FITS image Rectified 239s sky spectra 239s 239s No parameters 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_resample: 239s version 5.5.7 239s Parameters: {'dispersion': 0.0, 'startwavelength': 0.0, 'endwavelength': 0.0, 'flux': True} 239s Docstring: Resample input spectra at constant wavelength step 239s 239s This recipe is used to resample at constant wavelength step spatially 239s rectified spectra. The input frames are produced using either the 239s recipe fors_extract_slits in the case of MOS/MXU multi slit exposures, 239s or the recipes fors_remove_bias and fors_flatfield in the case of LSS 239s or long-slit like MOS/MXU data. Only in case of LSS or LSS-like data 239s the SLIT_LOCATION table is required in input. Please refer to the FORS 239s Pipeline User's Manual for more details. In the table below the MXU 239s acronym can also be read as MOS and LSS, SCI can be read as STD, and 239s SCIENCE as STANDARD. Input files: DO category: Type: 239s Explanation: Required: LAMP_UNBIAS_MXU or 239s SCIENCE_UNBIAS_MXU or SCIENCE_UNFLAT_MXU or RECTIFIED_LAMP_MXU 239s or RECTIFIED_ALL_SCI_MXU or RECTIFIED_SCI_MXU or 239s RECTIFIED_SKY_SCI_MXU Calib Frame to resample Y 239s DISP_COEFF_MXU or DISP_COEFF_SCI_MXU Calib Dispersion 239s coefficients Y SLIT_LOCATION_MXU Calib Slit location 239s table Y GRISM_TABLE Calib Grism table 239s . Output files: DO category: Data type: 239s Explanation: MAPPED_LAMP_MXU or MAPPED_ALL_SCI_MXU or 239s MAPPED_SCI_MXU or MAPPED_SKY_SCI_MXU FITS image Resampled 239s spectra 239s 239s Parameters: 239s dispersion: Expected spectral dispersion (Angstrom/pixel) 239s (float; default: 0.0) 239s startwavelength: Start wavelength in spectral extraction (float; 239s default: 0.0) 239s endwavelength: End wavelength in spectral extraction (float; 239s default: 0.0) 239s flux: Apply flux conservation (bool; default: True) 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_photometry: 239s version 5.5.7 239s 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} 239s Docstring: Compute corrected flatfield 239s 239s Input files: DO category: Type: Explanation: 239s Number: PHOT_TABLE FITS table Expected extinction 239s params 1 ALIGNED_PHOT FITS table Photometry 239s 1+ MASTER_SKY_FLAT_IMG FITS image Master flat field 239s 1 Output files: DO category: Data type: Explanation: 239s PHOT_COEFF_TABLE FITS image Observed extinction 239s coefficients CORRECTION_MAP FITS image Correction map 239s (magnitude) CORRECTION_FACTOR FITS image Correction map 239s (flux) MASTER_FLAT_IMG FITS image Corrected master flat 239s field 239s 239s Parameters: 239s fitz: Fit zeropoint (bool; default: True) 239s fit_all_mag: Always fit star magnitudes (bool; default: False) 239s fite: Fit atmospheric extinctions (str; default: 239s 'pernight') 239s fitc: Fit color correction term (bool; default: False) 239s use_all_stars: Use also non-standard stars to fit polynomial f 239s (bool; default: False) 239s degreef1: FLatfield correction map polynomial degree (x) (int; 239s default: 0) 239s degreef2: Flatfield correction map polynomial degree (y), or 239s negative for triangular coefficient matrix (int; 239s default: -1) 239s degreep: Extinction/color coupling degree (int; default: 0) 239s mjd_obs_target: MJD-OBS used to match the raw frame from which 239s EXTINCTION_PER_NIGHT and PHOT_COEFF inherit MJD-OBS. 239s If negative theMJD-OBS of the first raw frame isused 239s (float; default: -1.0) 239s Author: Jonas M. Larsen 239s 239s 239s Recipe fors_sumflux: 239s version 5.5.7 239s Parameters: {'xlow': 0, 'ylow': 0, 'xhigh': 0, 'yhigh': 0} 239s Docstring: Integrate flux from all or part of the input frame 239s 239s This recipe is used to monitor any lamp flux on the CCD. The input raw 239s image should be either a FLUX_ARC_LSS or a FLUX_FLAT_LSS frame. After 239s the background subtraction the total signal is integrated and divided 239s by the exposure time and by the total number of CCD original pixels 239s (keeping into account a possible rebinned readout). In the case of 239s FORS2 frames the background is the median level evaluated from the 239s available overscan regions. In the case of FORS1 data, where overscan 239s regions are missing, the background is evaluated as the median level 239s of the first 200 CCD columns for flat field data, while for arc lamp 239s data a background map evaluated from the regions without spectral 239s lines is computed and subtracted. The background subtracted frame is 239s written to output in all cases, and the QC parameters QC LAMP FLUX and 239s QC LAMP FLUXERR are computed. Input files: DO category: Type: 239s Explanation: Required: FLUX_FLAT_LSS Raw Flat 239s field exposure Y or FLUX_ARC_LSS Raw Arc lamp exposure 239s Y Output files: DO category: Data type: Explanation: 239s FLUX_LAMP_LSS FITS image Background subtracted integration region 239s 239s Parameters: 239s xlow: X coordinate of lower left corner of integration region 239s (pixel) (int; default: 0) 239s ylow: Y coordinate of lower left corner of integration region 239s (pixel) (int; default: 0) 239s xhigh: X coordinate of upper right corner of integration region 239s (pixel) (0 = CCD size) (int; default: 0) 239s yhigh: Y coordinate of upper right corner of integration region 239s (pixel) (0 = CCD size) (int; default: 0) 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_extract_slits: 239s version 5.5.7 239s Parameters: {'dispersion': 0.0, 'startwavelength': 0.0, 'endwavelength': 0.0, 'flux': True} 239s Docstring: Spatial rectification of spectral image 239s 239s This recipe is used to extract MOS/MXU slit spectra, following their 239s curvature, and to remap them into a spatially rectified image. Please 239s refer to the FORS Pipeline User's Manual for details about the spectra 239s remapping technique. Note however that the interpolation is done 239s exclusively along the spatial direction, and therefore the output 239s rectified image will have the same x size of the input spectral image. 239s In the table below the MXU acronym can be alternatively read as MOS. 239s Input files: DO category: Type: Explanation: 239s Required: LAMP_UNBIAS_MXU or SCIENCE_UNBIAS_MXU or 239s SCIENCE_UNFLAT_MXU or STANDARD_UNBIAS_MXU or STANDARD_UNFLAT_MXU 239s or UNMAPPED_SCI_MXU or UNMAPPED_STD_MXU or UNMAPPED_SKY_SCI_MXU 239s or UNMAPPED_SKY_STD_MXU Calib Spectral frame Y 239s SLIT_LOCATION_DETECT_MXU or SLIT_LOCATION_MXU Calib 239s Master flat frame Y CURV_COEFF_MXU Calib 239s Spectral curvature Y GRISM_TABLE Calib 239s Grism table . Output files: DO category: 239s Data type: Explanation: RECTIFIED_LAMP_MXU or 239s RECTIFIED_ALL_SCI_MXU or RECTIFIED_ALL_STD_MXU or 239s RECTIFIED_SCI_MXU or RECTIFIED_STD_MXU or RECTIFIED_SKY_SCI_MXU 239s or RECTIFIED_SKY_STD_MXU FITS image Rectified slit spectra 239s 239s Parameters: 239s dispersion: Expected spectral dispersion (Angstrom/pixel) 239s (float; default: 0.0) 239s startwavelength: Start wavelength in spectral extraction (float; 239s default: 0.0) 239s endwavelength: End wavelength in spectral extraction (float; 239s default: 0.0) 239s flux: Apply flux conservation (bool; default: True) 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_flatfield: 239s version 5.5.7 239s Parameters: {} 239s Docstring: Flat field correction of input frame 239s 239s This recipe is used to divide the input frame by the normalised flat 239s field frame produced by recipe fors_normalise_flat. The input frame 239s must be already bias subtracted (e.g., by recipe fors_remove_bias). In 239s the table below the MXU acronym can be alternatively read as MOS and 239s LSS. Input files: DO category: Type: 239s Explanation: Required: SCIENCE_UNBIAS_MXU or 239s STANDARD_UNBIAS_MXU Raw Bias subtracted frame Y 239s MASTER_NORM_FLAT_MXU Calib Normalised flat frame Y 239s Output files: DO category: Data type: Explanation: 239s SCIENCE_UNFLAT_MXU or STANDARD_UNFLAT_MXU FITS image Flat field 239s corrected frame 239s 239s No parameters 239s Author: Carlo Izzo 239s 239s 239s Recipe fors_img_sky_flat: 239s version 5.5.7 239s Parameters: {'stack_method': 'median', 'minrejection': 1, 'maxrejection': 1, 'klow': 3.0, 'khigh': 3.0, 'kiter': 999} 239s Docstring: Compute master img_sky_flat frame 239s 239s Input files: DO category: Type: Explanation: 239s Number: SKY_FLAT_IMG Raw Jittered sky flat 239s fields 1+ MASTER_BIAS FITS image Master bias 239s 1 Output files: DO category: Data type: Explanation: 239s MASTER_SKY_FLAT_IMG FITS image Master sky flat field 239s 239s Parameters: 239s stack_method: Frames combination method (str; default: 'median') 239s minrejection: Number of lowest values to be rejected (int; default: 239s 1) 239s maxrejection: Number of highest values to be rejected (int; default: 239s 1) 239s klow: Low threshold in ksigma method (float; default: 3.0) 239s khigh: High threshold in ksigma method (float; default: 3.0) 239s kiter: Max number of iterations in ksigma method (int; 239s default: 999) 239s Author: Jonas M. Larsen 239s 239s 239s autopkgtest [00:36:49]: test test-recipe.py: -----------------------] 240s autopkgtest [00:36:50]: test test-recipe.py: - - - - - - - - - - results - - - - - - - - - - 240s test-recipe.py PASS (superficial) 240s autopkgtest [00:36:50]: @@@@@@@@@@@@@@@@@@@@ summary 240s test-recipe.py PASS (superficial) 257s Creating nova instance adt-noble-s390x-cpl-plugin-fors-20240419-003250-juju-7f2275-prod-proposed-migration-environment-3-8a555430-b58f-4cdc-b33c-6bd5ce2c593d from image adt/ubuntu-noble-s390x-server-20240418.img (UUID 85e53509-ea4e-4742-afdb-a30c7e328507)...