3. SEDM Pipeline

3.1. Pipeline Overview

3.1.1. Python Requirements

The IFU pipeline is written in python v2.7 and currently runs under the miniconda2 distribution (https://conda.io/miniconda.html). It requires the astroconda environment from STScI (https://astroconda.readthedocs.io/en/latest/) and expects the name to be ‘astroconda’:

conda create -n astroconda stsci

There is no IRAF dependancy in the IFU pipeline, but the RCam pipeline still requires pyraf and the Ureka distribution.

The most up-to-date version of the IFU pipeline (as well as the RCam pipeline and database routines) can be found at github (https:github.com/scizen9/kpy.git).

3.1.2. Pipeline Operations

We are in the process of developing an automated system for data reduction and analysis. Currently, the only interactive step in the data reduction is placing the aperture(s) on the object(s). For transient followup, the data are usually taken in A/B pairs to improve the sky subtraction. This requires that the observer place an aperture on the A position (positive: red) and on the B position (negative: blue). See below for the interactive procedure. These steps may eventually be automated, depending on how robust and accurate our astrometry turns out to be.

Once the apertures have been placed, an ascii spectrum is automatically generated. The format of the ascii spectrum is universal enough to be input to any classifier (Superfit, e.g.), however, SNID is automatically run on iPTF targets at the end of the reduction run when a final report is generated. For iPTF targets, the final report generation also uploads the iPTF spectra to the marshal. This will change once the ZTF marshal comes online.

3.2. Automated Pipeline Operations

Before the observer interacts with the pipeline, the following steps are automatically performed:

  1. The appropriate reduced directory is created using the UT date:
    • /scr2/sedmdrp/redux/20151115 (e.g.)
  2. The required raw calibration files are copied over and reduced.
  3. If there is a failure in the reduction, calibrations files from previous runs are copied.
  4. All subsequent IFU images are automatically bias-subtracted, cosmic ray cleaned, and background subtracted.
  5. Any subsequent standard star IFU observations are reduced and extracted, and a flux calibration is generated.
  6. At the end of the night, all observations that can be automatically extracted are extracted (same as make auto).

3.3. Interactive Procedure

The observer connects with pharos either through VNC (recommended), or via an X enabled ssh connection (slower). Below is is a figure showing the layout of the desktop connected through the VNC connection.

_images/PharosSEDMdesktop.png

Figure 1. Pharos sedmdrp desktop on screen 7 (5907).

The automatic pipeline script is running in the bottom right window. Some status information can be gleaned from the output there. The xterm set on the left may be used by the observer to examine the files on pharos. A web browser will be set up on the desktop screen to the right which can be selected using the chooser on the lower right. This is where you can interact with the marshal.

Please be sure that the background subtraction has finished for the target you are reducing. This is the most time-consuming step. For each observation it will perform five iterations of traditional convolution, followed by an iteration of fast-Fourier convolution. For the A/B pairs, it will do this twice. Check the lower-right window to see if the background subtraction is in process.

We now record the name of the reducer (see step 7 below). This can be made easier if you set the environment variable SEDM_USER to your name in the top-right xterm window. It will then come up as the default name when asked.

In the top-right Xterm window, the observer interacts with the pipeline using the following steps:

  1. cd into current (UT) date directory:
    • cd /scr2/sedmdrp/redux/20151115 (e.g.)
  2. Confirm science targets:
    • grep science Makefile
    • A/B pairs will have target names like sp_PTF15drk.npy
    • if the pair has not finished the target name will be something like sp_PTF15drk_obs1_0.npy
    • do not process partial A/B pairs unless one has failed: the sky subtraction will be inferior
    • NOTE: if a target is bright, then only a single observation is made as the sky subtraction will not be as difficult.
  3. Initiate final reduction of science targets:
    • make science –> to make all science targets or
    • make sp_PTF15drk.npy –> to make a specific target (e.g.)
    • Note: targets that are already processed will not be re-done, so make science is a reasonable step after each pair has been read out.
  4. Scale the data cube:
    • Use ‘>’ and ‘<’ keys to adjust the A/B cube scaling limits until good visibility is obtained.
    • Hit ‘x’ to use new scale or ‘q’ to abandon adjustments and revert to default scaling.
_images/PTF15drk_Scale.png

Figure 2. Scaling the data cube for good visibility of targets.

  1. Place aperture on A target:
    • confer with PTF marshal cutouts and finder charts for the target object (e.g.)
    • find A object (positive: red)
    • place red aperture on target
    • adjust size with ‘z’ or ‘x’ keys
    • sky subtraction can be toggled on/off with the ‘y’ key (normally on)
    • left click when sized and placed
_images/PTF15drk_AperA.png

Figure 3. A/B Aperture placement: Aper A goes on positive (red) target.

  1. Place aperture on B target:
    • If A/B pair, find B object (negative: blue)
    • place red aperture on target
    • adjust size with ‘z’ or ‘x’ keys (should be same size as A)
    • left click when sized and placed
_images/PTF15drk_AperB.png

Figure 4. A/B Aperture placement: Aper B goes on negative (blue) target.

  1. The spectrum will be extracted and then displayed. When prompted, enter quality of observation based on the image and the extracted spectrum as follows:
    • 1 - good (no problems)
    • 2 - acceptable (minor problems, near neighbor, e.g.)
    • 3 - poor (major problems, A or B image missing, e.g.)
    • 4 - no object visible
    • NOTE: Only quality 1 and 2 will be uploaded to the marshal
    • After quality is entered, you will prompted to enter your name
_images/PTF15drk_SEDM.png

Figure 5. Extracted spectrum plot of PTF15drk, awaiting a quality.

  1. Completing step 7 will automatically generate an ascii spectrum and a pdf plot:
  2. Redo an object. If you wish to redo an object because of improper aperture placement, or for any other reason simply type:
    • make redo_PTF15drk (e.g., for A/B pair)
    • make redo_PTF15drk_obs1_0 (e.g., for a single-frame observation)
    • You can then re-place the aperture
  3. If you typed make science to initiate the data reduction, then an ascii report on the reductions is generated in the file report.txt. You can also re-generate it by typing make report.
  4. Most results and diagnostic plots are now automatically copied to the UT date subdirectory on the documentation web server in the directory linked here. Consult this page to check aperture placement, etc.
  1. When the night is complete, we now use an automatic script to perform a default classification (using SNID) and upload any resulting spectra with quality 1 or 2 to the marshal. To generate an e-mail report on the entire night of data reductions and initiate the automatic upload of the resulting good spectra to the marshal, please enter:
    • make finalreport

Last updated on 09 November 2017