README web version of /home/usg/OPS/MTS/readme_xml/readme_75008800

Principal Investigator Email Address

• fmarchis@berkeley.edu

Estimated Total Execution Time (hours, including overheads)

• 10

General Description

• We propose to study in detail the mysterious, rare, and short-lived
  volcanic outbursts seen on the surface of Io. Detection will be done
  using our alarm program on IRTF+Lick+Keck telescopes. As soon an event
  is detected, we will active this ToO program to observe in Io surface
  between 1-5 microns in 5 NB filters and in spectroscopy between 1-2.5
  microns with 2 spectro modes. This observation will be repeated three times
  two nights and four nights later to follow-up the eruption evolution 
  and nail down the highest temperature of the magma.

Waiver Requests

• On February 21, 2005, we submitted a Waiver for the use of several
  narrow band filters namely NB1.04, NB1.64, NB2.21, and NB4.05
  linked with the request of sky flat-fields in these narrow filters. It was 
  approved on February 22, 2005.
  From:   smengel@eso.org
  Subject: Waiver request 075.C-0088A.01.WAV approved
  Date: February 22, 2005 8:38:31 AM PST

Critical Observing Condition Constraints

• To nail down the highest temperature of the magma the observations
  must be taken ASAP, i.e in the night of the discovery of the eruption
  or considering the 46h orbital period of Io, two nights latter (the 
  same hemisphere will be approximatively seen).

Time-Critical Aspects

• N/A

Special Execution Requirements

• ---(Empty)---

Special Calibration Information

• ---(Empty)---

ToO Information

• Even if Io is a bright target (mv~5.8), it can be difficult to find it
  if it is located nearby Jupiter, and also because it cannot be easily
  differentiate from the other Galilean satellites. When the ToO will be
  activated, we will provide the support astronomer several displays of
  the Jovian system and a map showing Io and the position of the bright
  volcano. The eruption should anyway easily visible in imaging mode in
  K, Lp and NB4.05 band.  The slit should be located on the Io in a way
  that it is recorded at the same time the signal coming from the
  thermal emission of the active volcano and a nearby region without
  activity. The combinaison of both spectra will be used to isolate the
  pure thermal emission from the sunlit reflecting flux (see Fig. 3 of
  the proposal).
  
  The brightness of the outburst is unknown. I prepared two
  spectroscopic OBs based on an outburst reaching mK=6
  (IoBRIGHT_Spectro) and mK=7.5 (Io_Spectro). Following the characteristic
  of the new detector saturation can be avoid on the spectra. 
  Please, keep in mind that in case of extremely bright hot spot, it may be
  considered to use the N20C80 dichroic instead of the VIS one to avoid saturation.
   
  Note that in imaging mode, we should not face this problem thanks to the 
  Neutral density.

ToO Activators List

• Franck Marchis (fmarchis@berkeley.edu)
  Julie Rathbun (Julie_Rathbun@redlands.edu)

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 ?

• N/A

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

• N/A

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

• N/A

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

• YES

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

• N/A

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 have PSF reference star OBs, do the names of those OBs begin with
 PSF_ ?

• YES

If there are Finding Charts attached to your OBs, is the field-of-view
 of at least one of these charts 2' x 2' (with clearly labelled field orientation)
 ?

• N/A

Have you clearly marked and labelled your wavefront reference objects
 R1, R2, R3, ... (as specified in the NAOS Preparation Software) on your Finding
 Charts ?

• N/A

Have you specified the magnitude of the brightest object in the field-of-view
 for each OB ?

• YES

Are there objects in any of your fields (including standard stars) which
 are brighter than the limits specified in the User Manual and on NACO web Pages
 ?

• NO

If the previous answer is yes, have you given a list of OBs and a justification
 for the brightness limit violation in the general description field ?

• N/A