README web version of /home/usg/OPS/MTS/readme_xml/readme_83061300

Principal Investigator Email Address

• Jean-Louis.Monin@obs.ujf-grenoble.fr

Estimated Total Execution Time (hours, including overheads)

• 24h50mn

General Description

• This run addresses simultaneous spectroscopy of individual components
   in young binaries. 
  The binaries are tight, with separations between 0.1 and 2.0 arcsec, with a median
  separation value = 0.45 arcsec. 
  For each target, we provide the position angle of the binary in the OB, oriented
   from the primary. 
  The AO and SV guide stars are always the same, this is : the brightest star of every
   pair. 
  The PA is drawn on the finding charts, starting from the primary. 
  To get the 2 spectra simultaneously, the slit should be oriented along the binary
   PA. 
  In all cases, the OB are designed so that target = AO guide star = SV guide star.
   
  The median K magnitude difference between the primary and the secondary is dK=1.
   
  Hence the AO should be OK on the primary. In some rare cases the 2 stars are of
   very similar brightness
  but then the separation is very small. Look in the user comments for details on
   individual sources.
  
  We will observe at 3 wavelength setting : 
  Bracket gamma (2166 nm)
  Ca I triplet (2263 nm)
  CO lines (2293.2 nm)
  
  The first 2 settings above are free settings. We had a waiver approved on this question.
  Also, some of our blocks exceed the 1 hour time limit and we also have a waiver
   approved on this.
  
  In total, we have 3 waiver approved : 
  WaiverID:  083.C-0613A.01
  WaiverID:  083.C-0613A.02
  WaiverID:  083.C-0613A.03
  
  When running the VERIFY process, the verifcation fails but only because of reason
   concerning the waivers
  here above (exec time > 1 hour and 2 free settings + one on the acquisition).
  
  The observing method should be the following : identify the source from the Finding
   chart, and
  when the AO loop is closed, one should see the 2 components of the binary. 
  Then the slit should be aligned along the binary PA (look on the finding chart).
   
  
  There is one source that is going to be more tricky : ROXs 16 : this is a binary
   (AB) with sep=0.6, and 
  the A component (the brightest one) is itself a binary with sep 0.1''. There should
   be 2 observations of this object
  at 2 different PA (look at the OB). 
  
  If possible, the targets should be observed in the following (priority) order  :
   
  
  Elias 2-26
  AS 205
  SR 9
  Haro 1-4
  DOAr 24 E
  WSB 3
  ROXs 2
  V853 Oph
  WL 4
  YLW 16A 1 & 2
  SR 24 N
  DOAr 23
  ROXs 31
  YLW 19
  ROXs 16 AB
  ROXs 42 C
  SR 12
  ROXS 5
  VSSG 14
  ROXs 16 A-ab
  IRS 51
  
  For every object, we have chosen DIT values to get a S/N=50 (or so) at 2166nm, and
   70 (or so) at 2263 nm and 2293nm. 
  If the S/N is 20% lower than these values, the observation is OK. 
  Note that we use a free setting at 2166nm and at 2263 nm (waiver granted). We use
   a standard setting at 2293.2 nm.
  
  Calibrations (Telluric) : 
  We have only 2 Telluric stars situated very close to our targets (they are all gathered
   in a small part of the sky, average RA = 16:20, average DEC = -24.
  We have duplicated the calibration OBS to put them in the middle of the science
   OB list with names CAL_. We use the same PA orientation of the
   slit
  (SKY position) for the science OB and for the CAL_ star.
  The Telluric stars are both A0V stars with V very close to 7. The S/N in 10s should
   be of the order of 50 at 2166 and 2263, 2293.2

Waiver Requests

• Three waiver requests were submitted and granded :
  WaiverID:  083.C-0613A.01
  WaiverID:  083.C-0613A.02
  WaiverID:  083.C-0613A.03
  
  They concern the use of free wavelength settings and the fact that some OBS are
   a bit over 1 hour exec time.

Critical Observing Condition Constraints

• No real critical observing constraints are requested. We request the seeing
   to be good (0.6'') but not extremely good, because we observe binaries that can
   be very
  tight and we need the AO correctionto be good.

Time-Critical Aspects

• No time critical aspect in term of coordinated observations for instance.
  On the other hand, we would like some short science OBs (20-30 mn exec time) to
   be performed back to back with only one telluric star to calibrate both, because
   
  20 telluric stars x 20 mn adds 6 hours to our exec time that we did not take into
   account at preparation time.

Special Execution Requirements

• None

Special Calibration Information

• ---(Empty)---

ToO Information

• ---(Empty)---

ToO Activators List

• ---(Empty)---

Do the README file and the instrument comments of the telluric stars
 OBs include the required S/N/pixel of the spectrum of the telluric star, its spectral
 type and allowed spectral range?

• YES

Do any OBs include wavelength or flatfield calibrations?

• NO

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

• N/A

If the slit viewer guide star is different from the target, are the RA
 and DEC offsets accurate to within 0.05 arcsec and do they take into account the
 relative proper motion between the two objects?

• N/A

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

• YES