README web version of /home/usg/OPS/MTS/readme_xml/readme_77013600

Principal Investigator Email Address

• peter@astro.su.se

Estimated Total Execution Time (hours, including overheads)

• 9.0

General Description

• This is a ToO program which attempts to detect narrow emission lines
  at the earliest observable phases of a type Ia supernova (SN Ia). The observations
  should be taken as soon as possible after triggering (if possible
  within the first week after the SN explosion).

Waiver Requests

• A waiver request for OBs exceeding 1 hour was granted with the restriction
   that
  if the conditions degrade after the first hour, the OB will not be repeated.

Critical Observing Condition Constraints

• none

Time-Critical Aspects

• The observations should be taken as soon as possible after the ToO triggering.

Special Execution Requirements

• The number of follow-ups depends on whether we detect narrow lines on
   the
  first observation, or not. All this is accounted for in the OBs and will be
  specified in detail when the programme is triggered.
  
  The first epoch observations for a SNIa or for a supernova with
  an unknown type:
  
  3 x 1050 seconds with DIC1 (390+564)
  3 x 1050 seconds with DIC2 (437+760)
  
  The follow-up observations depend on whether or not the narrow CSM lines
  were detected in the first epoch. If there was a narrow line detection, the
  SN will be followed-up 7 and 14 days later with the following sequence of
  observations:
  
  6 x 1320sec with DIC1 (390+564)
  
  If no CSM lines were detected in the first epoch, a second much deeper
  observation will follow as soon as possible after the first one:
  
  8 x 1800 seconds with DIC1 (390+564)
  
  NOTE: the total time of the submitted OBs exceeds the allocation by
  the OPC. However, we will only make use of subsets of the OBs, i.e.
  either follow the first epoch by a second much deep epoch, or two
  less deep epochs. Each branch individually complies with the time
  limit given to us.
  
  A finding chart will be supplied with the trigger of the programme.
  
  All the OBs of a given epoch are not identical. Observations with a wide slit
  (3.0") have been included in some of the OBs to allow for absolute flux calibration
   
  of the observations.

Special Calibration Information

• A spectrophotometric standard star close to the supernova should be observed
  with the same instrument settings as the supernova on each epoch the
  supernova is observed. The spectrophotometric standard star observations with
  DIC1 will also be carried out with a wide (3.0") slit to allow for absolute
  flux calibration for the science spectrum. In addition, telluric standard
  stars should be observed together with the deep (8 x 1800 sec) SNIa spectra
  such that one standard star (spectrophot. or telluric) is observed close in
  time and airmass to each of the science OBs. We will select suitable
  spectrophotometric and telluric standards, and provide the details together
  with the finding chart when triggering the ToO observations for a given
  supernova.
  
  We have attached flat field observations of 2x8sec (RED) and 2x12sec (BLUE)
  to each DIC1 OB in the first epoch SN observation and in the deep follow-up epoch
   for
  a type Ia SN in which no narrow lines were detected. For the first epoch DIC2 OBs
  flat field observations of 2x22sec (RED) and 2x15sec (BLUE) were attached.
  These are necessary in order to obtain optimal correction for the possible instrumental
   effects (telluric lines arising within the spectrograph and CCD fringing).

ToO Information

• This is a ToO program. It should be activated by an early nearby supernova.
   
  The PI (Lundqvist), or CoI's Leibundgut, Mattila or Sollerman, will contact 
  the observatory when such an object has been discovered and will provide the 
  exact coordinates. A finding chart will be provided, if available, but the 
  offsets from the galaxy nucleus plus the brightness of the object should make 
  the acquisition unambiguous.

ToO Activators List

• The PI (Lundqvist), or CoI's Leibundgut, Mattila or Sollerman

Is this a Pre-imaging run ?

• false

Pre-imaging Requirements

• ---(Empty)---

Source(s) of Pre-imaging

• ---(Empty)---

Pre-imaging sources not listed above

• ---(Empty)---

Do all your OBs comply with the instrument-specific requirements listed
 on the instrument-specific Phase 2 web page ?

• YES

If this is a pre-imaging run, did you select PRE-IMAGING for the Observing
 Category for each Observing Template ?

• N/A

Do all your finding charts comply with both the general and instrument-specific
 Phase 2 Web Pages ?

• YES

If you submitted OBs for standard stars, did you specify the magnitude
 and spectral type of all standard stars in the OBs ?

• YES

Have you included OBs for any calibrations that you need but which are
 not part of the Calibration Plan ?

• YES

If you are observing Moving Targets, have you attached suitable ephemeris
 files to your OBs?

• N/A

If you have preferences which OBs should be executed first, did you make
 use of the User Priority field in the OBs ?

• YES

If this is a run that requires coordinated observations with other facilities,
 did you give proper instructions in the Time-Critical Aspects Section ?

• N/A

If you need secondary guiding, are there suitable objects within 30 arcsec
 from your target ?

• N/A