README web version of /home/usg/OPS/MTS/readme_xml/readme_77073801

Principal Investigator Email Address

```
tboeker@rssd.esa.int
```

Estimated Total Execution Time (hours, including overheads)

```
5 hours
```

General Description

We will use SINFONI in its H+K configuration to obtain R~1600 spectra
 of the inner circum-nuclear starburst ring in NGC 5248. The ring is visible only
 in emission lines maps and has a diameter of about 2". We use SINFONI in non-AO
 mode. Target acquisition occurs on the galaxy nucleus itself which should be obvious
 in the acquisition images because it is by far the brightest NIR source in the field.
 Because the ring fills a fair fraction of the 8"x8" FOV, the nucleus (i.e. the peak
 of the NIR light)
should be well-centered in the SINFONI field, and the jitter range should be small
 (no more than 1"). Because the host galaxies are rather large on the sky, we require
 a large nod amplitude of typically a few arcmin, and hence use the FixedSkyOffset
 nodding
mode.
The nucleus of NGC 5248 is the brightest source in the field. Our best estimate
 for the central surface brightness is derived from the 2MASS H-band image. The range
 for the peak SB is 12 < mu_H < 14 mags/sqarcsec. This should be far from detector
 saturation in the DIT=300s long integrations.

Waiver Requests

```
No Waiver Request was submitted
```

Critical Observing Condition Constraints

We require good seeing conditions (0.8" or better) because spatial resolution
 is crucial to separate the various "hot spots" in the rings. Because absolute flux
 calibration is less crucial, photometric conditions are not required, although the
 sky background
should be as stable as possible in order to allow accurate correction of telluric
 lines.

Time-Critical Aspects

There are no time-critical aspects to our observations.

Special Execution Requirements

```
not applicable
```

Special Calibration Information

Our program requires no special calibrations except the standard observation
 of telluric standard stars, which should preferrably be hot stars of spectral type
 B5 or hotter.

ToO Information

```
not applicable
```

ToO Activators List

```
not applicable
```

Is this a Pre-imaging run ?

```
false
```

Pre-imaging Requirements

```
not applicable
```

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 ?

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?

```
N/A
```

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

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
```

Did you indicate the magnitude of the brightest object in the field in each SINFONI OB?

If you are using the AO: Did you indicate for every OB the magnitude of the guide star, and its distance to the target (if any)?

```
N/A
```

If you submitted OBs for standard stars, did you use the provided StandardStar templates?

```
N/A
```

If you are using a specific offset pattern or position angle: did you check carefully the definition in the manual?

```
N/A
```

Did you make really sure that none of your OBs ever saturates the detector?

If you are using the AO: did you enter the correct Strehl Ratio (on-axis, K-band) AND the seeing value in the constraint set?

```
N/A
```

Last creation of page: Tue Oct 6 15:40:14 2009
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