README web version of /home/usg/OPS/MTS/readme_xml/readme_76005500

Principal Investigator Email Address

```
dsilva@eso.org
```

Estimated Total Execution Time (hours, including overheads)

```
90.5 hours
```

General Description

HISTORY:
    Version 1: August 2005 - original
    Version 2: 14 Nov 2005 - 
               Updated information about large proper motion objects (Highlight
 6) 
               Updated information about faint (V < 9) stars (Highlight 8)
               Updated information about crowded fields (Highlight 8)
               As appropriate, added finding charts (see Highlight 6 and 8)
    Version 3: 18 Nov 2005 - 
               Added OBs for 20 O/B stars
               Updated information about crowded fields (Highlight 8)

HIGHLIGHTS:

(1) Number of Stars in Period 76 sample: 132 + 3 telluric absorption
    standards. Number of OBs per star: 2 (DIC1 and DIC2), except where
    noted below.

(2) "Filler" program: stars can be observed in any order under any
    conditions.  Please try to observe at seeing better than 2
    arcsecs.

(3) Please try to observe the DIC1 and DIC2 OBs for each star on the
    same night.

(4) Please observe one (1) telluric star every other month.  Please
    separate the telluric star observations by approximately one (1) month.
    Please observe the telluric stars at airmass ~ 1.5.

(5) The execution time of most OBs is much less than one (1) hour.  A
    few OBs have execution times as long as 80 minutes.

(6) Some stars have large proper motions. For these stars,
    coordinates have been corrected for proper motion to
    epoch 2006.0. Finding charts for the epoch 2006.0 position
    have been attached - the object in question should be 
    at the center of the finding chart. The large proper motion
    objects are:

    HD 33793
    HD 63077
    HD 106516
    HD 114710
    V_UV_Cet


(7) Some of the cooler stars (spectral types KM) are probably
    variable.  Please confirm that the TiO peaks in these objects are
    not saturated.

(8) For stars with V < 9 *or* in crowded fields, finding
    charts have been attached. The desired stars are in the
    center of the finding chart. These stars are:

    SAO 180855
    HD 34797
    HD 36960
    HD 48279
    HD 193281
    HD 195434
    HD 205811

(9) If Paranal needs more OBs later in the semester, we have more
    stars to observe. :-)

OVERVIEW:

Title: HST Next General Spectral Library: A UVES Followup (Part 5)

The Next Generation Spectral Library (NGSL) was an HST Snapshot
project to use STIS to obtain spectra spanning the HR diagram in four
separate metallicity bins.  This library will be used mainly to model
the integrated spectral energy distributions of unresolvable stellar
systems.  During HST Cycles 10 - 13, Gregg et al. (including Silva)
obtained STIS spectra for 382 stars in four metallicity bins.  These
STIS spectra have spectral range 170 -- 1030 nm, with resolution ~1000
at all wavelengths.

The goal of this on-going UVES "filler" programme is to obtain
followup high-resolution spectra with UVES for the 240 stars visible
from Paranal.  To date, UVES spectra for 107 stars have been obtained
and processed.

These UVES spectra will be used to verify the stellar atmospheric
parameters of the NGSL stars, to construct high-resolution synthetic
stellar population models, and as a comprehensive reference library
for stellar atmosphere modelers.  This program complements and extends
the Paranal Observatory Program (POP), primarily by providing a
metal-poor extension.  Analogous with the NGST STIS data, these new
UVES data will be made public immediately.

For each star, two UVES setup are used: DIC1 (346+580) and DIC2
(437+860).  We wish to obtain R ~ 48000 at all wavelengths.  To
achieve this, the following slit widths (in arcsecs) are used: (346,
437, 580, 860) :: (1.0, 1.0, 0.90, 0.90).

Our Signal-to-Noise (SNR) goals are 100 - 250 per pixel (or greater)
at all wavelengths.  Using UVES ETC 2.8.6, extensive simulations as a
function of magnitude and spectral type have been executed using a
Slit = 1.0 arcsec and Full Moon.  Exposure times have been selected to
achieve maximum possible SNR without saturation at 0.5 arcsec seeing
and Airmass = 1.  For redder stars (KM), care was taken to avoid
saturation at TiO peaks.

Of course, since this is a "filler" programme, most observations will
be done at higher airmass and worse seeing.  At constant airmass, SNR
will will decrease by factor of 1.5 (approximately) if seeing changes
from 0.5 to 2.0, as summarised here:

               Airmass = 2
                Seeing
               --------
               0.5  2.0

    346        150  100
    437        400  267
    580 (AFG)  300  200
    580 (KM)   250  167
    860 (AFG)  300  200
    860 (KM)   350  167

For constant seeing, SNR will change by 1.14 in the blue and not
change in the red as airmass changes from 1 to 2, as summarised here:

         Air=1 Air=2
         ----- -----
    346  140   100
    437  115   100
    580  106   100
    860  100   100

Most OB execution times are much less than one (1) hour.  A few OBs
have execution times as long as 80 minutes.  

Star co-ordinates and proper motions have been extracted from Simbad.
All co-ordinates and proper motions are for equinox and epoch 2000.
Some stars have large proper motions.  Proper motions were entered
into OB Target Package.  Co-ordinates have *not* been corrected for
proper motion for the mean epoch.

Many of the OBs have NEXPOBLUE and/or NEXPORED set to 2 or 3.
Multiple exposures are used to reach SNR goals and/or improve cosmic
ray rejection.  In particular, no individual exposure time is longer
than 45 minutes (2700 secs).

Waiver Requests

WAIVER 71.B-0529A.01: permission granted to omit finding charts for
bright, isolated stars where identification during acquisition is
unambiguous. We have assumed this wavier continues for Period 76.

Using DSS cut-outs, a 3x3 arcmin box around each star
has been examined. Finding charts have been provided
for: (1) stars with V < 9; (2) stars in crowded fields;
and (3) stars with large proper motion. See General
Discussion section for more details and lists of affected
stars.

Critical Observing Condition Constraints

```
Nothing special here.
```

Time-Critical Aspects

TELLURIC TARGETS: as explained in the next section, three (3) telluric
absorption OBs have been submitted - one star for November, January,
and March.  The names of these OBs start with TELLURIC XXX where XXX
is the month.  Their Time Intervals have been set appropriately.

SCIENCE TARGETS (DIC1+DIC2 TOGETHER): as noted above, each object
needs to be observed in two settings: DIC1 (346+580) and DIC2
(437+860).  Whenever possible, please execute both settings for a
single object on a single night.  Objects can be variable (especially
the cooler stars), so it would be good to get complete wavelength
coverage at the same phase.  A few fainter objects have multiple for
each setting.  For these objects, please try to observe DIC1+DIC2
pairs on a single night.  It would be good (but certainly not
mandatory!) to observe all the pairs for a single star on a single
night.

TARGETS WITH DEC > +20: There are a small number of objects with Dec >
+20.  These have more narrow time windows when airmass < 2.5 than the
rest of the sample.

Special Execution Requirements

SCIENCE TARGETS (DIC1+DIC2 TOGETHER): as noted above, each object
needs to be observed in two settings: DIC1 (346+580) and DIC2
(437+860).  Whenever possible, please execute both settings for a
single object on a single night.  Objects can be variable (especially
the cooler stars), so it would be good to get complete wavelength
coverage at the same phase.  A few fainter objects have multiple for
each setting.  For these objects, please try to observe DIC1+DIC2
pairs on a single night.  It would be good (but certainly not
mandatory!) to observe all the pairs for a single star on a single
night.

Special Calibration Information

Attached Flats have been requested for all observations to obtain the
best possible flat-field correction.  This is particularly important
for fringe-correction in the red.

Ideally, each OB would be followed by an observation of a hot star to
measure the current telluric absorption strength.  In practice, this
is too time consuming for a project where random stars will be
observed on random nights.  Using data from the Archive, tests have
demonstrated that telluric absorption can be corrected at the ~ 2%
level even using observations widely separated in time.  Therefore, a
different B star will be observed in DIC1 and DIC2 every other month
to measure telluric absorption.  This yields three (3) stars and six
(6) OBs.  IMPORTANT: please observe these stars at Airmass ~ 1.5.

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 ?

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 ?

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

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 ?

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

```
N/A
```

Last creation of page: Tue Oct 6 15:40:09 2009
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