README web version of /home/usg/OPS/MTS/readme_xml/readme_75020101

Principal Investigator Email Address

• marcello.fulchignoni@obspm.fr

Estimated Total Execution Time (hours, including overheads)

• 8h

General Description

• We want to continuosly investigate the asteroid Steins, target of the
   Rosetta space mission, during its rotational period (about 6.1 hours), for a total
   exp. time of 8 consecutive hours, comprising solar analog observations for the removal
   of the solar contribution. We want to repeat VBRIV imaging observations followed
   by a spectral acquisition, alternating 2 different grism (#2 and #4), covering the
   whole asteroid rotational period. For our purpose we need a photometric nigth. The
   strategy is to start with a photometric sequence (OB:2867Steins_photA_1) , then
   acquire a spectrum with Gr2 (OB: 2867Steins_specGR2_1), then another photometric
   sequence (OB: 2867Steins_photB_1) and finally the spectrum with GR4 (OB: 2867Steins_specGr4_1).
   This sequence of 4 OB takes about 40 minutes and must be continuosly repeated for
   the 8 hours allocated of observing time; we provide 9 sequences with these 4 OB
   (_2, .._9), plus some OB with only photometry. Ephemeris must be inserted according
   to the eph. file. During the observations, we need also some solar analog spectral
   acquisition (Ob are provided) once about 1 hour.

Waiver Requests

• No Waiver Request was submitted

Critical Observing Condition Constraints

• Target identification: we provide some finder charts for possible observing
   nigths already scheduled in service. If not enough, the strategy to identify the
   target (mag around 16th) is the following: take an OB with a photometric sequence
   (2867Steins_photA_init); take a solar analog star OB (Solar_HD144585_1), take another
   photometric sequence on the target (2867Steins_photA_1). The time passing between
   the first V image on the target and the last one must be enough to clearly identify
   the moving target. To confirm, an ESO DSS image of the field could help, the asteroid
   must be the additional object in the Field of view respect the DSS background stars.
   In http://asteroid.lowell.edu/cgi-bin/koehn/astfinder, putting the name of the ast.
   "Steins", you will have the finder chart for the date

Time-Critical Aspects

• Our target must be observed in the July-September period, when it is visible
   enougth time to be investigated during its full rotational period. The month of
   August, if possible, is preferred for the asteroid phase angle configuration

Special Execution Requirements

• We need to continuosly repeat the following sequence of 4 OB (photometry+spectroscopyGR2+
   photometry + SpectrGR4, for a total time of about 40m) continuously during the 8
   allocated hours of observing time: 2867Steins_photA_n, 2867Steins_specGr2_n, 2867Steins_photB_n,
   2867Steins_specGr4_n, where n goes from 1 to 9 (we foreseen that 9 sequences with
   the 4 OB could be executed). The sequences of OBs on the target must be interrupted
   about once an hour to acquire a solar analog spectrum as indicated in the Special
   calib. information.
  Please note that ephemeris and differential tracking for Steins must be updated
   at the UT and date of observations, according to the given ephemeris file.

Special Calibration Information

• We need a standard calibration plan plus the observation of solar analog
   stars (spectroscopy): for these last, OBs are provided together with our targets.
   We need one solar analog (SA) observation every 50-70 minutes: considering the required
   observing period, the first useful SA is HD144585 that could be taken at the beginning
   of the nigth and 1 hour later, than Land112-1333 (about 3 and 4 hours after the
   beginning of observations), then LA115-271 (5 and 6 hours after the beg. of obs)
   and finally HD1835 (around 7 hours after the beg. of obs and at the end). Please
   note that these stars must be acquired with airmass not higher than 1.6
  In the standard calibration plan, we need bias, dome flat (spectroscopy, slit 2",
   gr 2 and 4), twiligth flats (B-V-R-I), 1 spectrophotometric std (Gr 2 and 4) and
   several landolt fields for absolute photometric calibration. Please take at least
   4 Landolt field at different airmass, taking eventually some Landolt acquisitions
   also during the "science" allocated time (we have foreseen some obs. time for this
   in our plan).

ToO Information

• ---(Empty)---

ToO Activators List

• ---(Empty)---

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?

• 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