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The Michelle software has been substantially reworked for Semester 04A. In particular there are changes to the acquisition sequence, which are reflected in the details of the Observing Tool library for Michelle. This document shows some Michelle specific items not covered in the normal user guide to the OT. It assumes that you have read that generic guide. It also discusses a Michelle specific acquisition method - peakup after imaging acquire. At the summit, MSBs are now executed via the "Observing Queue", which is detailed in the execution manual.
LibraryThe OT library for Michelle is divided into several subsections, as shown in Figure 1.
Imaging
For imaging mode, all you have to do in the target component is select the appropriatefilter. If you want to shorten or lengthen the time taken in each nod beam, then you can also alter the observation time. The default 20 seconds for observation time actually means 20 seconds total in each chop beam (including array readout overheads). Therefore, the default setting will give approximately 40 seconds in each nod beam, or 160 seconds total for a nodded ABBA sequence. The target component also provides the detector duty cycle in percent. Use this number to estimate the actual exposure time in each chop beam. E.g., if the detector duty cycle is 80%, then approximately 16 seconds out of the 20 second observation time is spent exposing on the source. NB. Exposure times are sky-dependent and rarely need to be changed. On the odd occasion that an exposure time needs reducing because the target is extremely bright, or you are carrying out a classically scheduled run in poor conditions, please refer to the list of working exposure times to choose a more appropriate exposure time. Target information: Both the chop position angle (degrees east of north) and throw (arcsecs) are set in the target component, as this is an input to the telescope system rather than the instrument. The default chop angle is 0 degrees (north-south) with a throw of 15 arcsecs. The maximum chop throw while guiding is 21.7 arcsecs, the unguided maximum throw is about 30 arcsecs, but depends on the temperature of the top end. Chop frequency is determined automatically by the software and cannot be changed by the observer.
Repeats: To calculate how many times you should repeat a typical ABBA pattern, please refer to the tables in "Estimating the number of repeats required in a Michelle observing sequence". Offsets: Typical offsets for point source imaging are perpendicular to the chop angle and half the distance of the chop throw. This means that the source will always appear on the array even in the negative chop position, and the resulting ABBA pattern will produce a "square" chopping and nodding patter, as shown in Fig 3. Be sure to leave the final offset iterator in the sequence, i.e., the one after the observe. This moves the telescope back to your 0,0 position, and is also required by the data reduction. Flatfields: The actual benefit of taking flatfields in the mid-IR for imaging programmes is questionable, although you can set them up in your programme if you want to. Bear in mind that the imaging data reduction recipes will not use any flatfields your produce and that this will have to be done offline. To set up a flatfield sequence, simply copy one of the normal imaging sequences and replace the observation component with a flat component. Make sure you open the flat component and hit default (the flat source should by "sky"). You can offset the telescope as you would a normal observation, or stare at one piece of sky - the choice is yours. Remember that if you want to use a particular piece of sky, you can enter the coordinates in the target component. Alternatively, if you want to point the telescope to the east for instance, and take flats at airmasses of 1, 1.5 and 2, you can specify azimuth and elevation angles in the target component. Overheads: Typical overheads for Si filter imaging are 100%, i.e., 10 minutes on source requires 20 minutes overall. Broad band filters, because of the short exposure time needed, result in much larger overheads of approximately 200 to 250%. Spectroscopy
Although the observation time in this component has the same definition as in imaging, the situation is more complicated due to detector sampling. The observation time gives the total time spent in each chop beam (including overheads) per sample position. Therefore, you may consider reducing the observation time to 10 seconds if you are using sampling of 1x2 (which moves the detector a distance of one pixel in order to remove bad pixels on the array) as this will give you approximately 40 seconds in one nod beam, or 160 seconds for an ABBA sequence. If you decide to select the default observation time of 20 seconds and use 1x2 sampling, then you will spend 80 seconds in each nod beam, or 320 seconds for the ABBA sequence. With 2x2 sampling you should almost certainly reduce the observation time to 10 seconds or less. With the observation time set to 20 seconds, 2x2 sampling will result in a nod position that lasts for 160 seconds and you will almost certainly see problems due to thermal instability. The instrument component will also provide an estimated detector duty cycle which is the percentage of time actually spent exposing on a source in each .chop beam Use this number to estimate the total exposure time on your target. Target component: We recommend that you put the standard star information in the target component at the top of the MSB, and your target information in the target component within the science target sequence. The telescope will then slew to the standard when doing the flatfield and remain there for the standard star observation. It will slew to the target once these two observations have been made. The chop throw and position angle are also set in the target component. As mentioned above, if you want to chop along the slit, make sure that the chop position angle in the target component is the same as the slit position angle in the instrument component.
Repeats: To calculate how many times you should repeat a typical ABBA pattern, please refer to the tables in "Estimating the number of repeats required in a Michelle observing sequence". Nod iterator: One major change we have made to the sequences as compared to 2001/2002 is the use of nod iterators in spectroscopy sequences, as opposed to offset iterators. This makes setting up your spectroscopy sequence simpler, in that you do not have to specify telescope nod offsets. The nod iterator allows you to choose from two option, AB or ABBA. The default is ABBA which gives four observations for each sequence. Use the repeat option to increase the number of times the pattern is repeated to increase signal to noise. The nod iterator uses the chop throw and angle settings to nod the telescope along the slit with the same throw as the chop. Typical resulting data are shown in Fig. 4. The offset iterator can still be used if you want more flexibility for the telescope nod positions, and are by default used in the MSB for nodding and chopping off the slit, and also in the echelle MSBs since the echelle does not utilize chopping. Overheads: Expect total overheads of 100% for low resolution spectroscopy and perhaps as low as 50% for medium to high resolution spectroscopy. For bright sources, target acquisition should add two or three minutes to the total observation time. Arcs: Arc lamp spectra are not currently used with Michelle, sky lines are used instead. These come for free in your individual chop beams so there is no need to set up anything specific for wavelength calibration. The data reduction will also produce sky frames which you can use for offline wavelength calibration. Target acquisition:
The user simply has to hit the default button in this component. Since only one filter is used for target acquisition, the exposure time is fixed and cannot be changed by the user. However, if the target is relatively faint, the number of coadds can be increased. At the time of writing, this mode of acquisition has not been fully tested and so the limiting magnitude for acquisition is unknown. However, 30 coadds should be enough to detect a 650 mJy source sufficiently well for acquisition. Adjust the coadds as necessary depending on the brightness of your source, but do not drop the coadds below about 10 since this might result in poor chop subtraction. At the telescope, the observer also has another chance to do a traditional peakup through the slit after target acquisition to ensure that the source is well positioned on the slit. If you are want to make sure the source is as accurately positioned as possible, you should mention in your observing note in the OT that the observer should check the peakup position. PolarimetryImaging polarimetry and spectropolarimetry are covered in one section here. For specific information about imaging and spectroscopy setups, please refer to the sections above.
Instrument component: The only differences between imaging/spectroscopy setups and those for polarimetry are that 1) the polarimetry box at the top of the component should be ticked and that 2) the exposure times will be longer in most cases due to the reduction in throughput caused by the waveplates. The exposure times will automatically default to the correct values if the polarimetry box is ticked. Target component: There is no difference in the target component when doing polarimetry. However, you may wish to limit the chop throw for point sources as the waveplates offer a limited field of view of approximately 40 arcsecs in Michelle's current mode. IRPOL iterator: For consistency within the OT, Michelle uses the IRPOL waveplate iterator in its sequences. However, Michelle has its own polarimetry module in the calibration unit and the iterator will control this rather than the IRPOL unit itself. There is no need to specify which polarimetry module is used, the observing software does this automatically. Please leave the final IRPOL iterator in the sequence (after the final offset of 0,0 in imaging mode) as this will move the waveplates back to their 0 angle position.
Programme checklist for PIs and support scientist
vetting
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